<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Ahn, Christopher P.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Barkhouser, Robert H.</style></author><author><style face="normal" font="default" size="100%">Bautista, Julian E.</style></author><author><style face="normal" font="default" size="100%">Beifiori, Alessandra</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bhardwaj, Vaishali</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blake, Cullen H.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Blomqvist, Michael</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Borde, Arnaud</style></author><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Brown, Peter J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Bundy, Kevin</style></author><author><style face="normal" font="default" size="100%">Busca, N. G.</style></author><author><style face="normal" font="default" size="100%">Carithers, William</style></author><author><style face="normal" font="default" size="100%">Carnero, Aurelio R.</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Chen, Yanmei</style></author><author><style face="normal" font="default" size="100%">Comparat, Johan</style></author><author><style face="normal" font="default" size="100%">Connolly, Natalia</style></author><author><style face="normal" font="default" size="100%">Cope, Frances</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz N.</style></author><author><style face="normal" font="default" size="100%">Davenport, James R. A.</style></author><author><style face="normal" font="default" size="100%">Delubac, Timothée</style></author><author><style face="normal" font="default" size="100%">de Putter, Roland</style></author><author><style face="normal" font="default" size="100%">Dhital, Saurav</style></author><author><style face="normal" font="default" size="100%">Ealet, Anne</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett L.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Escoffier, S.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Filiz Ak, N.</style></author><author><style face="normal" font="default" size="100%">Finley, Hayley</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Génova-Santos, R.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Haggard, Daryl</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Harris, Ben</style></author><author><style face="normal" font="default" size="100%">Harris, David W.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holder, Diana</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Huehnerhoff, Joe</style></author><author><style face="normal" font="default" size="100%">Jordan, Beatrice</style></author><author><style face="normal" font="default" size="100%">Jordan, Wendell P.</style></author><author><style face="normal" font="default" size="100%">Kauffmann, Guinevere</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal A.</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Klaene, Mark A.</style></author><author><style face="normal" font="default" size="100%">Kneib, Jean-Paul</style></author><author><style face="normal" font="default" size="100%">Le Goff, Jean-Marc</style></author><author><style face="normal" font="default" size="100%">Lee, Khee-Gan</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio A. 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Jordan</style></author><author><style face="normal" font="default" size="100%">Rebolo, Rafael</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Roe, Natalie A.</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Rossi, Graziano</style></author><author><style face="normal" font="default" size="100%">Rubiño-Martin, J. 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G.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shen, Yue</style></author><author><style face="normal" font="default" size="100%">Shu, Yiping</style></author><author><style face="normal" font="default" size="100%">Slosar, Anže</style></author><author><style face="normal" font="default" size="100%">Smee, Stephen A.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stauffer, Fritz</style></author><author><style face="normal" font="default" size="100%">Steele, Oliver</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Streblyanska, Alina</style></author><author><style face="normal" font="default" size="100%">Suzuki, Nao</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Tal, Tomer</style></author><author><style face="normal" font="default" size="100%">Tanaka, Masayuki</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, M.</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Viel, Matteo</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Watson, Mike</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Weiner, Benjamin J.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. M.</style></author><author><style face="normal" font="default" size="100%">Yeche, Christophe</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author><author><style face="normal" font="default" size="100%">Zheng, Zheng</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Baryon Oscillation Spectroscopic Survey of SDSS-III</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmology: observations;  surveys</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013AJ....145...10D</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">145</style></volume><pages><style face="normal" font="default" size="100%">10</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The Baryon Oscillation Spectroscopic Survey (BOSS) is designed tomeasure the scale of baryon acoustic oscillations (BAO) in theclustering of matter over a larger volume than the combined efforts ofall previous spectroscopic surveys of large-scale structure. BOSS uses1.5 million luminous galaxies as faint as i = 19.9 over 10,000deg&lt;SUP&gt;2&lt;/SUP&gt; to measure BAO to redshifts z &lt; 0.7. Observations ofneutral hydrogen in the Lyα forest in more than 150,000 quasarspectra (g &lt; 22) will constrain BAO over the redshift range 2.15 &lt;z &lt; 3.5. Early results from BOSS include the first detection of thelarge-scale three-dimensional clustering of the Lyα forest and astrong detection from the Data Release 9 data set of the BAO in theclustering of massive galaxies at an effective redshift z = 0.57. Weproject that BOSS will yield measurements of the angular diameter</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1208.0022</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Parejko, John K.</style></author><author><style face="normal" font="default" size="100%">Sunayama, Tomomi</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">van den Bosch, Frank</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz Alberto Nicolaci</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Don</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey E.</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Wetzel, Andrew</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zheng, Zheng</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: the low-redshift sample</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">large-scale structure of Universe;  galaxies: haloes;  galaxies: evolution;  galaxies: statistics;  surveys</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013MNRAS.429...98P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">429</style></volume><pages><style face="normal" font="default" size="100%">98-112</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We report on the small-scale (0.5 &lt; r &lt; 40 h&lt;SUP&gt;-1&lt;/SUP&gt; Mpc)clustering of 78 895 massive (M&lt;SUB&gt;*&lt;/SUB&gt; ˜ 10&lt;SUP&gt;11.3&lt;/SUP&gt;M&lt;SUB&gt;&amp;sun;&lt;/SUB&gt;) galaxies at 0.2 &lt; z &lt; 0.4 from the first twoyears of data from the Baryon Oscillation Spectroscopic Survey (BOSS),to be released as part of Sloan Digital Sky Survey (SDSS) Data Release 9(DR9). We describe the sample selection, basic properties of thegalaxies and caveats for working with the data. We calculate the real-and redshift-space two-point correlation functions of these galaxies,fit these measurements using halo occupation distribution (HOD)modelling within dark matter cosmological simulations, and estimate theerrors using mock catalogues. These galaxies lie in massive haloes, witha mean halo mass of 5.2 × 10&lt;SUP&gt;13&lt;/SUP&gt; h&lt;SUP&gt;-1&lt;/SUP&gt;M&lt;SUB&gt;&amp;sun;&lt;/SUB&gt;, a large-scale bias of ˜2.0 and a satellitefraction of 12 ± 2 per cent. Thus, these galaxies occupy haloeswith average masses in between those of the higher redshift BOSS CMASSsample and the original SDSS I/II luminous red galaxy sample.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1211.3976</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Carnero, Aurelio</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Raccanelli, Alvise</style></author><author><style face="normal" font="default" size="100%">Aubourg, Eric</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz A. N.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett</style></author><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, Mariana</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Montesano, Francesco</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Sheldon, Alaina</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmology: observations;  (cosmology:) inflation;  (cosmology:) large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013MNRAS.428.1116R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">428</style></volume><pages><style face="normal" font="default" size="100%">1116-1127</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We analyse the density field of 264 283 galaxies observed by the SloanDigital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey(BOSS) and included in the SDSS Data Release 9 (DR9). In total, the SDSSDR9 BOSS data include spectroscopic redshifts for over 400 000 galaxiesspread over a footprint of more than 3000 deg&lt;SUP&gt;2&lt;/SUP&gt;. We measurethe power spectrum of these galaxies with redshifts 0.43 &lt; z &lt; 0.7in order to constrain the amount of local non-Gaussianity,f{_N_L^local}, in the primordial density field, paying particularattention to the impact of systematic uncertainties. The BOSS galaxydensity field is systematically affected by the local stellar densityand this influences the ability to accurately measure f{_N_L^local}. Inthe absence of any correction, we find (erroneously) that theprobability that f{_N_L^local} is greater than zero, P(f{_N_L^local}&gt; 0), is 99.5 per cent. After quantifying and correcting for thesystematic bias and including the added uncertainty, we find - 45 &lt;f{_N_L^local} &lt; 195 at 95 per cent confidence and P(f{_N_L^local}&gt; 0) = 91.0 per cent. A more conservative approach assumes that wehave only learnt the k dependence of the systematic bias and allows anyamplitude for the systematic correction; we find that the systematiceffect is not fully degenerate with that of f{_N_L^local}, and wedetermine that -82 &lt; f{_N_L^local} &lt; 178 (at 95 per centconfidence) and P(f{_N_L^local} &gt; 0) = 68 per cent. This analysisdemonstrates the importance of accounting for the impact of Galacticforegrounds on f{_N_L^local} measurements. We outline the methods thataccount for these systematic biases and uncertainties. We expect ourmethods to yield robust constraints on f{_N_L^local} for both our ownand future large-scale structure investigations.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1208.1491</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Aird, James</style></author><author><style face="normal" font="default" size="100%">Coil, Alison L.</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Diamond-Stanic, Aleksandar M.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Kenneth C. Wong</style></author><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">PRIMUS: An observationally motivated model to connect the evolution of the AGN and galaxy populations out to z~1</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013arXiv1301.1689A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1301</style></volume><pages><style face="normal" font="default" size="100%">1689</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present an observationally motivated model to connect the AGN andgalaxy populations at 0.2&lt;z&lt;1.0 and predict the AGN X-rayluminosity function (XLF). We start with measurements of the stellarmass function of galaxies (from the Prism Multi-object Survey) andpopulate galaxies with AGNs using models for the probability of a galaxyhosting an AGN as a function of specific accretion rate (the rate ofsupermassive black hole growth scaled relative to the host stellarmass). Our model is based on measurements indicating that the specificaccretion rate distribution is a universal function across a wide rangeof host stellar mass with slope gamma_1=0.65 and an overallnormalization that evolves strongly with redshift. We test severalsimple assumptions to extend this model to high specific accretion rates(beyond the measurements) and compare the predictions for the XLF withthe observed data. We find good agreement with a model that allows for abreak in the specific accretion rate distribution at a pointcorresponding to the Eddington limit, with a steep power-law tail tosuper-Eddington ratios with slope gamma_2=-2.1 +0.3 -0.5. We convertbetween specific accretion rate and Eddington ratio by assuming ascaling between black hole mass and host stellar mass with an intrinsicscatter of +/-0.38 dex. Our results show that samples of low luminosityAGNs are dominated by moderately massive galaxies (M* ~ 10^{10-11}M_sun) growing with a wide range of accretion rates -- a consequence ofthe shape of the galaxy stellar mass function rather than a preferencefor AGN activity at a particular stellar mass. The observed populationof the most luminous AGN may be severely skewed to the most extremesources with elevated black hole masses relative to their host galaxiesand in rare phases of very rapid accretion.</style></abstract><notes><style face="normal" font="default" size="100%">11 pages, 5 figures, emulateapj format, submitted to ApJ</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1301.1689</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Coil, Alison</style></author><author><style face="normal" font="default" size="100%">Aird, James</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Mendez, Alexander J.</style></author><author><style face="normal" font="default" size="100%">Kenneth C. Wong</style></author><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author><author><style face="normal" font="default" size="100%">Arnouts, Stephane</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">PRIMUS: Constraints on Star Formation Quenching and Galaxy Merging, and the Evolution of the Stellar Mass Function From z=0-1</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013arXiv1301.1688M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1301</style></volume><pages><style face="normal" font="default" size="100%">1688</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We measure the evolution of the stellar mass function (SMF) from z=0-1using multi-wavelength imaging and spectroscopic redshifts from thePRism MUlti-object Survey (PRIMUS) and the Sloan Digital Sky Survey(SDSS). From PRIMUS we construct an i&lt;23 flux-limited sample of~40,000 galaxies at z=0.2-1.0 over five fields totaling ~5.5 deg^2, andfrom the SDSS we select ~170,000 galaxies at z=0.01-0.2 that we analyzeconsistently with respect to PRIMUS to minimize systematic errors in ourevolutionary measurements. We find that the SMF of all galaxies evolvesrelatively little since z=1, although we do find evidence for mass</style></abstract><notes><style face="normal" font="default" size="100%">submitted to ApJ; revised to reflect first referee report; 39 emulateapj pages, 20 figures, 7 tables</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1301.1688</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Kepler, S. O.</style></author><author><style face="normal" font="default" size="100%">Koester, D.</style></author><author><style face="normal" font="default" size="100%">Pelisoli, Ingrid</style></author><author><style face="normal" font="default" size="100%">Peçanha, Viviane</style></author><author><style face="normal" font="default" size="100%">Nitta, A.</style></author><author><style face="normal" font="default" size="100%">Costa, J. E. S.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, J.</style></author><author><style face="normal" font="default" size="100%">Dufour, P.</style></author><author><style face="normal" font="default" size="100%">Lachapelle, F.-R.</style></author><author><style face="normal" font="default" size="100%">Bergeron, P.</style></author><author><style face="normal" font="default" size="100%">Yip, Ching-Wa</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Althaus, L.</style></author><author><style face="normal" font="default" size="100%">Córsico, A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS DR7 White Dwarf Catalog</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">catalogs;  magnetic fields;  stars: luminosity function;  mass function;  surveys;  white dwarfs</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013ApJS..204....5K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">204</style></volume><pages><style face="normal" font="default" size="100%">5</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present a new catalog of spectroscopically confirmed white dwarfstars from the Sloan Digital Sky Survey (SDSS) Data Release 7spectroscopic catalog. We find 20,407 white dwarf spectra, representing19,712 stars, and provide atmospheric model fits to 14,120 DA and 1011DB white dwarf spectra from 12,843 and 923 stars, respectively. Thesenumbers represent more than a factor of two increase in the total numberof white dwarf stars from the previous SDSS white dwarf catalogs basedon DR4 data. Our distribution of subtypes varies from previous catalogsdue to our more conservative, manual classifications of each star in ourcatalog, supplementing our automatic fits. In particular, we find alarge number of magnetic white dwarf stars whose small Zeeman splittingsmimic increased Stark broadening that would otherwise result in anoverestimated log g if fit as a non-magnetic white dwarf. We calculatemean DA and DB masses for our clean, non-magnetic sample and find the DBmean mass is statistically larger than that for the DAs.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1212.1222</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tassev, Svetlin</style></author><author><style face="normal" font="default" size="100%">Zaldarriaga, Matias</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Solving Large Scale Structure in Ten Easy Steps with COLA</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013arXiv1301.0322T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1301</style></volume><pages><style face="normal" font="default" size="100%">322</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present the COmoving Lagrangian Acceleration (COLA) method: an N-bodymethod for solving for Large Scale Structure (LSS) in a frame that iscomoving with observers following trajectories calculated in LagrangianPerturbation Theory (LPT). Unlike standard N-body methods, the COLAmethod can straightforwardly trade accuracy at small-scales in order togain computational speed without sacrificing accuracy at large scales.This is especially useful for cheaply generating large ensembles ofaccurate mock halo catalogs required to study galaxy clustering and weaklensing, as those catalogs are essential for performing detailed erroranalysis for ongoing and future surveys of LSS. As an illustration, weran a COLA-based N-body code on a box of size 100Mpc/h with particles ofmass ~5*10^9Msolar/h. Running the code with only 10 timesteps wassufficient to obtain an accurate description of halo statistics down tohalo masses of at least 10^11Msolar/h. This is only at a modest speedpenalty when compared to mocks obtained with LPT. A standard detailedN-body run is orders of magnitude slower than our COLA-based code. Thespeed-up we obtain with COLA is due to the fact that we calculate thelarge-scale dynamics exactly using LPT, while letting the N-body codesolve for the small scales, without requiring it to capture exactly theinternal dynamics of halos. Achieving a similar level of accuracy inhalo statistics without the COLA method requires at least 3 times moretimesteps than when COLA is employed.</style></abstract><notes><style face="normal" font="default" size="100%">18 pages, 7 figures</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1301.0322</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">García Pérez, Ana E.</style></author><author><style face="normal" font="default" size="100%">Cunha, Katia</style></author><author><style face="normal" font="default" size="100%">Shetrone, Matthew</style></author><author><style face="normal" font="default" size="100%">Majewski, Steven R.</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Smith, Verne V.</style></author><author><style face="normal" font="default" size="100%">Schiavon, Ricardo P.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon</style></author><author><style face="normal" font="default" size="100%">Nidever, David</style></author><author><style face="normal" font="default" size="100%">Zasowski, Gail</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, Peter M.</style></author><author><style face="normal" font="default" size="100%">Girardi, Léo</style></author><author><style face="normal" font="default" size="100%">Hearty, Fred R.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Meszaros, Szabolcs</style></author><author><style face="normal" font="default" size="100%">O'Connel, Robert W.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Robin, Annie C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schultheis, Mathias</style></author><author><style face="normal" font="default" size="100%">Skrutskie, Michael F.</style></author><author><style face="normal" font="default" size="100%">Simmonsand, Audrey</style></author><author><style face="normal" font="default" size="100%">Wilson, John C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Very Metal-poor Stars in the Outer Galactic Bulge Found by the Apogee Survey</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Solar and Stellar Astrophysics;  Astrophysics - Galaxy Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2013</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2013</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2013arXiv1301.1367G</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1301</style></volume><pages><style face="normal" font="default" size="100%">1367</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Despite its importance for understanding the nature of early stellargenerations and for constraining Galactic bulge formation models, atpresent little is known about the metal-poor stellar content of thecentral Milky Way. This is a consequence of the great distances involvedand intervening dust obscuration, which challenge optical studies.However, the Apache Point Observatory Galactic Evolution Experiment(APOGEE), a wide-area, multifiber, high-resolution spectroscopic surveywithin Sloan Digital Sky Survey III (SDSS-III), is exploring thechemistry of all Galactic stellar populations at infrared wavelengths,with particular emphasis on the disk and the bulge. An automatedspectral analysis of data on 2,403 giant stars in twelve fields in thebulge obtained during APOGEE commissioning yielded five stars with lowmetallicity([Fe/H]$\le-1.7$), including two that are very metal-poor[Fe/H]$\sim-2.1$ by bulge standards. Luminosity-based distance estimatesplace the five stars within the outer bulge, where other 1,246 of theanalyzed stars may reside. A manual reanalysis of the spectra verifiesthe low metallicities, and finds these stars to be enhanced in the$\alpha$-elements O, Mg, and Si without significant $\alpha$-patterndifferences with other local halo or metal-weak thick-disk stars ofsimilar metallicity, or even with other more metal-rich bulge stars.While neither the kinematics nor chemistry of these stars can yetdefinitively determine which, if any, are truly bulge members, ratherthan denizens of other populations co-located with the bulge, thenewly-identified stars reveal that the chemistry of metal-poor stars inthe central Galaxy resembles that of metal-weak thick-disk stars atsimilar metallicity.</style></abstract><notes><style face="normal" font="default" size="100%">6 pages, 3 figures, 2 tables</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1301.1367</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Scalzo, Richard</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">Mehta, Kushal T.</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A 2 per cent distance to z = 0.35 by reconstructing baryon acoustic oscillations - I. Methods and application to the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmological parameters;  cosmology: observations;  dark energy;  distance scale;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.427.2132P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">427</style></volume><pages><style face="normal" font="default" size="100%">2132-2145</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present the first application to density field reconstruction to agalaxy survey to undo the smoothing of the baryon acoustic oscillation(BAO) feature due to non-linear gravitational evolution and therebyimprove the precision of the distance measurements possible. We applythe reconstruction technique to the clustering of galaxies from theSloan Digital Sky Survey (SDSS) Data Release 7 (DR7) luminous red galaxy(LRG) sample, sharpening the BAO feature and achieving a 1.9 per centmeasurement of the distance to z = 0.35. We update the reconstructionalgorithm of Eisenstein et al. to account for the effects of surveygeometry as well as redshift-space distortions and validate it on 160LasDamas simulations. We demonstrate that reconstruction sharpens theBAO feature in the angle averaged galaxy correlation function, reducingthe non-linear smoothing scale Σ&lt;SUB&gt;nl&lt;/SUB&gt; from 8.1 to 4.4 Mpch&lt;SUP&gt;-1&lt;/SUP&gt;. Reconstruction also significantly reduces the effects ofredshift-space distortions at the BAO scale, isotropizing thecorrelation function. This sharpened BAO feature yields an unbiaseddistance estimate (&lt;0.2 per cent) and reduces the scatter from 3.3 to2.1 per cent. We demonstrate the robustness of these results to thevarious reconstruction parameters, including the smoothing scale, thegalaxy bias and the linear growth rate. Applying this reconstructionalgorithm to the SDSS LRG DR7 sample improves the significance of theBAO feature in these data from 3.3σ for the unreconstructedcorrelation function to 4.2σ after reconstruction. We estimate arelative distance scale D&lt;SUB&gt;V&lt;/SUB&gt;/r&lt;SUB&gt;s&lt;/SUB&gt; to z = 0.35 of 8.88± 0.17, where r&lt;SUB&gt;s&lt;/SUB&gt; is the sound horizon andDV≡(DA2H-1)1/3 is a combination of the angular diameter distanceD&lt;SUB&gt;A&lt;/SUB&gt; and Hubble parameter H. Assuming a sound horizon of 154.25Mpc, this translates into a distance measurement D&lt;SUB&gt;V&lt;/SUB&gt;(z = 0.35)= 1.356 ± 0.025 Gpc. We find that reconstruction reduces thedistance error in the DR7 sample from 3.5 to 1.9 per cent, equivalent toa survey with three times the volume of SDSS.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1202.0090</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Mehta, Kushal T.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A 2 per cent distance to z = 0.35 by reconstructing baryon acoustic oscillations - II. Fitting techniques</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmological parameters;  cosmology: observations;  cosmology: theory;  distance scale;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.427.2146X</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">427</style></volume><pages><style face="normal" font="default" size="100%">2146-2167</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present results from fitting the baryon acoustic oscillation (BAO)signal in the correlation function obtained from the first applicationof density-field reconstruction to a galaxy redshift survey, namely theSloan Digital Sky Survey (SDSS) Data Release 7 (DR7) luminous red galaxy(LRG) catalogue. Reconstruction works to partially remove the effects ofnon-linear structure growth on the BAO by reconstructing the linearmatter density field from the observed galaxy density field using thecontinuity equation. We also introduce more careful approaches forderiving a suitable covariance matrix and fitting model for galaxycorrelation functions. Our covariance matrix technique guarantees smoothdiagonal and off-diagonal terms by fitting a modified Gaussiancovariance matrix to that calculated from mock catalogues. Our proposedfitting model is effective at removing broad-band effects such asredshift-space distortions, scale-dependent bias and any artefactsintroduced by assuming the wrong model cosmology. These all aid inobtaining a more accurate measurement of the acoustic scale and itserror. We validate these techniques on 160 mock catalogues derived fromthe LasDamas simulations in real and redshift space. We then apply thesetechniques to the DR7 LRG sample and find that the error on the acousticscale decreases from ˜3.5 per cent before reconstruction to˜1.9 per cent after reconstruction. We also see an increase in ourBAO detection confidence from ˜3σ to ˜4σ afterreconstruction with our confidence level in measuring the correctacoustic scale increasing from ˜3σ to ˜5σ. Usingthe mean of the acoustic scale probability distributions produced fromour fits, we find D&lt;SUB&gt;v&lt;/SUB&gt;/r&lt;SUB&gt;s&lt;/SUB&gt; = 8.89 ± 0.31before reconstruction and 8.88 ± 0.17 after reconstruction.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1202.0091</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Mehta, Kushal T.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A 2 per cent distance to z = 0.35 by reconstructing baryon acoustic oscillations - III. Cosmological measurements and interpretation</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmological parameters;  cosmology: observations;  cosmology: theory;  distance scale;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.427.2168M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">427</style></volume><pages><style face="normal" font="default" size="100%">2168-2179</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We use the 2 per cent distance measurement from our reconstructed baryonacoustic oscillations (BAOs) signature using the Sloan Digital SkySurvey (SDSS) Data Release 7 (DR7) luminous red galaxies fromPadmanabhan et al. and Xu et al. combined with cosmic microwavebackground data from Wilkinson Microwave Anisotropy Probe (WMAP7) tomeasure parameters for various cosmological models. We find a 1.7 percent measurement of H&lt;SUB&gt;0&lt;/SUB&gt; = 69.8 ± 1.2 km s&lt;SUP&gt;-1&lt;/SUP&gt;Mpc&lt;SUP&gt;-1&lt;/SUP&gt; and a 5.0 per cent measurement ofΩm=0.280±0.014 for a flat universe with a cosmologicalconstant. These measurements of H&lt;SUB&gt;0&lt;/SUB&gt; and Ω&lt;SUB&gt;m&lt;/SUB&gt;are robust against a range of underlying models for the expansionhistory. We measure the dark energy equation of state parameter w =-0.97 ± 0.17, which is consistent with a cosmological constant.If curvature is allowed to vary, we find that the Universe is consistentwith a flat geometry (Ω&lt;SUB&gt;K&lt;/SUB&gt; = -0.004 ± 0.005). Wealso use a combination of the 6 Degree Field Galaxy Survey BAO data,WiggleZ Dark Energy Survey data, Type Ia supernovae data and a localmeasurement of the Hubble constant to explore cosmological models withmore parameters. Finally, we explore the effect of varying the energydensity of relativistic particles on the measurement of H&lt;SUB&gt;0&lt;/SUB&gt;.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1202.0092</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Saito, Shun</style></author><author><style face="normal" font="default" size="100%">Reid, Beth</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">de Putter, Roland</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz Alberto Nicolaci</style></author><author><style face="normal" font="default" size="100%">Gott, J. Richard, III</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Oravetz, Dan</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">de Simoni, Fernando</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Acoustic Scale from the Angular Power Spectra of SDSS-III DR8 Photometric Luminous Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">distance scale;  cosmological parameters;  cosmology: observations;  large-scale structure of universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...761...13S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">761</style></volume><pages><style face="normal" font="default" size="100%">13</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We measure the acoustic scale from the angular power spectra of theSloan Digital Sky Survey III (SDSS-III) Data Release 8 imaging catalogthat includes 872, 921 galaxies over ~10,000 deg&lt;SUP&gt;2&lt;/SUP&gt; between0.45 &lt; z &lt; 0.65. The extensive spectroscopic training set of theBaryon Oscillation Spectroscopic Survey luminous galaxies allows preciseestimates of the true redshift distributions of galaxies in our imagingcatalog. Utilizing the redshift distribution information, we buildtemplates and fit to the power spectra of the data, which are measuredin our companion paper, to derive the location of Baryon acousticoscillations (BAOs) while marginalizing over many free parameters toexclude nearly all of the non-BAO signal. We derive the ratio of theangular diameter distance to the sound horizon scale D&lt;SUB&gt;A&lt;/SUB&gt;(z)/r&lt;SUB&gt;s&lt;/SUB&gt; = 9.212&lt;SUP&gt;+0.416&lt;/SUP&gt; &lt;SUB&gt;- 0.404&lt;/SUB&gt; at z= 0.54, and therefore D&lt;SUB&gt;A&lt;/SUB&gt; (z) = 1411 ± 65 Mpc at z =0.54; the result is fairly independent of assumptions on the underlyingcosmology. Our measurement of angular diameter distance D&lt;SUB&gt;A&lt;/SUB&gt;(z) is 1.4σ higher than what is expected for the concordanceΛCDM, in accordance to the trend of other spectroscopic BAOmeasurements for z &gt;~ 0.35. We report constraints on cosmologicalparameters from our measurement in combination with the WMAP7 data andthe previous spectroscopic BAO measurements of SDSS and WiggleZ. Werefer to our companion papers (Ho et al. de Putter et al.) forinvestigations on information of the full power spectrum.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1201.2172</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Assef, R. J.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Jones, C.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Forman, W. R.</style></author><author><style face="normal" font="default" size="100%">Dey, A.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, A. H.</style></author><author><style face="normal" font="default" size="100%">Green, P.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">AGES: The AGN and Galaxy Evolution Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmology: observations;  galaxies: evolution;  galaxies: general;  quasars: general</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJS..200....8K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">200</style></volume><pages><style face="normal" font="default" size="100%">8</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The AGN and Galaxy Evolution Survey (AGES) is a redshift surveycovering, in its standard fields, 7.7 deg&lt;SUP&gt;2&lt;/SUP&gt; of the Boötesfield of the NOAO Deep Wide-Field Survey. The final sample consists of23,745 redshifts. There are well-defined galaxy samples in 10 bands (theB&lt;SUB&gt;W&lt;/SUB&gt; , R, I, J, K, IRAC 3.6, 4.5, 5.8, and 8.0 μm, and MIPS24 μm bands) to a limiting magnitude of I &lt; 20 mag forspectroscopy. For these galaxies, we obtained 18,163 redshifts from asample of 35,200 galaxies, where random sparse sampling was used todefine statistically complete sub-samples in all 10 photometric bands.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1110.4371</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Assef, R. J.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Jones, C.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Forman, W. R.</style></author><author><style face="normal" font="default" size="100%">Dey, A.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, A. H.</style></author><author><style face="normal" font="default" size="100%">Green, P.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</style></title><secondary-title><style face="normal" font="default" size="100%">VizieR Online Data Catalog</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Active gal. nuclei;  Galaxies: IR;  Photometry: infrared;  Photometry: ultraviolet;  Redshifts;  QSOs;  Surveys</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012yCat..22000008K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">220</style></volume><pages><style face="normal" font="default" size="100%">00008</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The observations were made with Hectospec, a 300 fiber, 1 degree fieldof view, robotic spectrograph for the 6.5m MMT telescope at Mt. Hopkins,from 2004 April to 2007 July. The wavelength range is 3700-9200Åwith a pixel scale of 1.2Å and a spectral resolution of 6Å(i.e., roughly R~1000).(7 data files).</style></abstract><notes><style face="normal" font="default" size="100%">table2.dat 133x85 The spectroscopic observations; table5.dat 40810x61 *Summary of selection codes and flags; table6.dat 40810x103 Magnitudes and fluxes; table7.dat 40810x91 Redshifts; table8.dat 40810x72 Photometric redshifts; table9.dat 40810x53 Completeness and K-corrections for the galaxy; samples ; codes.dat 33x283 Sample selection binary code explanations</style></notes></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Nidever, David L.</style></author><author><style face="normal" font="default" size="100%">Zasowski, Gail</style></author><author><style face="normal" font="default" size="100%">Majewski, Steven R.</style></author><author><style face="normal" font="default" size="100%">Bird, Jonathan</style></author><author><style face="normal" font="default" size="100%">Robin, Annie C.</style></author><author><style face="normal" font="default" size="100%">Martinez-Valpuesta, Inma</style></author><author><style face="normal" font="default" size="100%">Beaton, Rachael L.</style></author><author><style face="normal" font="default" size="100%">Schönrich, Ralph</style></author><author><style face="normal" font="default" size="100%">Schultheis, Mathias</style></author><author><style face="normal" font="default" size="100%">Wilson, John C.</style></author><author><style face="normal" font="default" size="100%">Skrutskie, Michael F.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Robert W.</style></author><author><style face="normal" font="default" size="100%">Shetrone, Matthew</style></author><author><style face="normal" font="default" size="100%">Schiavon, Ricardo P.</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Weiner, Benjamin</style></author><author><style face="normal" font="default" size="100%">Gerhard, Ortwin</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Sellgren, Kris</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, Peter M.</style></author><author><style face="normal" font="default" size="100%">Elia García Pérez, Ana</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon</style></author><author><style face="normal" font="default" size="100%">Hearty, Fred R.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Apache Point Observatory Galactic Evolution Experiment: First Detection of High-velocity Milky Way Bar Stars</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Galaxy: bulge;  Galaxy: kinematics and dynamics;  Galaxy: structure;  surveys</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...755L..25N</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">755</style></volume><pages><style face="normal" font="default" size="100%">L25</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Commissioning observations with the Apache Point Observatory GalacticEvolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III,have produced radial velocities (RVs) for ~4700 K/M-giant stars in theMilky Way (MW) bulge. These high-resolution (R ~ 22, 500), high-S/N(&gt;100 per resolution element), near-infrared (NIR; 1.51-1.70 μm)spectra provide accurate RVs (epsilon&lt;SUB&gt;V&lt;/SUB&gt; ~ 0.2 kms&lt;SUP&gt;-1&lt;/SUP&gt;) for the sample of stars in 18 Galactic bulge fieldsspanning -1° &lt;l &lt; 20°, |b| &lt; 20°, and δ &gt;-32°. This represents the largest NIR high-resolution spectroscopicsample of giant stars ever assembled in this region of the Galaxy. Acold (σ&lt;SUB&gt;V&lt;/SUB&gt; ~ 30 km s&lt;SUP&gt;-1&lt;/SUP&gt;), high-velocity peak (V&lt;SUB&gt;GSR&lt;/SUB&gt; ≈ +200 km s&lt;SUP&gt;-1&lt;/SUP&gt;) is found to comprise a</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1207.3797</style></custom3><reprint-edition><style face="normal" font="default" size="100%">unexplained.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Busca, Nicolás G.</style></author><author><style face="normal" font="default" size="100%">Delubac, Timothée</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Le Goff, J.-M.</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Slosar, Anze</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Bautista, Julian E.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blomqvist, Michael</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Borde, Arnaud</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Carithers, Bill</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Lee, Khee-Gan</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Margala, Daniel</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Mehta, Kushal</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, Jordi</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Noterdaeme, Pasquier</style></author><author><style face="normal" font="default" size="100%">Olmstead, Matthew D.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Roe, N. A.</style></author><author><style face="normal" font="default" size="100%">Rollinde, Emmanuel</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Rossi, Graziano</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin S.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Viel, Matteo</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Yèche, Christophe</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Baryon Acoustic Oscillations in the Ly-\alpha\ forest of BOSS quasars</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012arXiv1211.2616B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1211</style></volume><pages><style face="normal" font="default" size="100%">2616</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We report a detection of the baryon acoustic oscillation (BAO) featurein the three-dimensional correlation function of the transmitted fluxfraction in the \Lya forest of high-redshift quasars. The study uses48,640 quasars in the redshift range $2.1\le z \le 3.5$ from the BaryonOscillation Spectroscopic Survey (BOSS) of the third generation of theSloan Digital Sky Survey (SDSS-III). At a mean redshift $z=2.3$, wemeasure the monopole and quadrupole components of the correlationfunction for separations in the range $20\hMpc&lt;r&lt;200\hMpc$. A peakin the correlation function is seen at a separation equal to$(1.01\pm0.03)$ times the distance expected for the BAO peak within aconcordance $\Lambda$CDM cosmology. This first detection of the BAO peakat high redshift, when the universe was strongly matter dominated,results in constraints on the angular diameter distance $\da$ and theexpansion rate $H$ at $z=2.3$ that, by themselves, require the existenceof dark energy. Combined with constraints derived from Cosmic MicrowaveBackground (CMB) observations, this result implies$H(z=2.3)=(224\pm8){\rm km s^{-1}Mpc^{-1}}$, indicating that the timederivative of the cosmological scale parameter $\dot{a}=H(z=2.3)/(1+z)$is significantly greater than that measured with BAO at $z\sim0.5$. Thisdemonstrates that the expansion was decelerating in the range$0.7&lt;z&lt;2.3$, as expected from the matter domination during thisepoch. Combined with measurements of $H_0$, one sees the pattern ofdeceleration followed by acceleration characteristic of a dark-energydominated universe.</style></abstract><notes><style face="normal" font="default" size="100%">submitted to Astronomy and Astrophysics</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1211.2616</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Connolly, Natalia</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Pandey, Parul</style></author><author><style face="normal" font="default" size="100%">Seitz, Stella</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. Michael</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The BOSS Emission-Line Lens Survey (BELLS). I. A Large Spectroscopically Selected Sample of Lens Galaxies at Redshift ~0.5</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...744...41B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">744</style></volume><pages><style face="normal" font="default" size="100%">41</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a catalog of 25 definite and 11 probable strong galaxy-galaxygravitational lens systems with lens redshifts 0.4 &amp;lt;~ z &amp;lt;~ 0.7,discovered spectroscopically by the presence of higher-redshift emissionlines within the Baryon Oscillation Spectroscopic Survey (BOSS) ofluminous galaxies, and confirmed with high-resolution Hubble SpaceTelescope (HST) images of 44 candidates. Our survey extends themethodology of the Sloan Lens Advanced Camera for Surveys survey (SLACS)to higher redshift. We describe the details of the BOSS spectroscopiccandidate detections, our HST ACS image processing and analysis methods,and our strong gravitational lens modeling procedure. We report BOSSspectroscopic parameters and ACS photometric parameters for allcandidates, and mass-distribution parameters for the best-fit singularisothermal ellipsoid models of definite lenses. Our sample to date wasselected using only the first six months of BOSS survey-qualityspectroscopic data. The full five-year BOSS database should produce asample of several hundred strong galaxy-galaxy lenses and in combinationwith SLACS lenses at lower redshift, strongly constrain the redshiftevolution of the structure of elliptical, bulge-dominated galaxies as afunction of luminosity, stellar mass, and rest-frame color, therebyproviding a powerful test for competing theories of galaxy formation andevolution.Based on observations made with the NASA/ESA Hubble Space Telescope,obtained at the Space Telescope Science Institute, which is operated bythe Association of Universities for Research in Astronomy, Inc., underNASA contract NAS 5-26555. These observations are associated withprogram 12209. Based on spectroscopic data from the Baryon OscillationSpectroscopic Survey of the Sloan Digital Sky Survey III.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1112.3683</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Shu, Yiping</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Connolly, Natalia</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Arneson, Ryan A.</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The BOSS Emission-Line Lens Survey. II. Investigating Mass-density Profile Evolution in the SLACS+BELLS Strong Gravitational Lens Sample</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">galaxies: elliptical and lenticular;  cD;  galaxies: evolution;  galaxies: structure;  gravitational lensing: strong</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...757...82B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">757</style></volume><pages><style face="normal" font="default" size="100%">82</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present an analysis of the evolution of the central mass-densityprofile of massive elliptical galaxies from the SLACS and BELLS stronggravitational lens samples over the redshift interval z ≈ 0.1-0.6,based on the combination of strong-lensing aperture mass and stellarvelocity-dispersion constraints. We find a significant trend towardsteeper mass profiles (parameterized by the power-law density model withρvpropr &lt;SUP&gt;-γ&lt;/SUP&gt;) at later cosmic times, with magnitude d&lt; γ &gt; /dz = -0.60 ± 0.15. We show that the combinedlens-galaxy sample is consistent with a non-evolving distribution ofstellar velocity dispersions. Considering possible additional dependenceof &lt;γ &gt; on lens-galaxy stellar mass, effective radius, andSérsic index, we find marginal evidence for shallower massprofiles at higher masses and larger sizes, but with a significance thatis subdominant to the redshift dependence. Using the results ofpublished Monte Carlo simulations of spectroscopic lens surveys, weverify that our mass-profile evolution result cannot be explained bylensing selection biases as a function of redshift. Interpreted as atrue evolutionary signal, our result suggests that major dry mergersinvolving off-axis trajectories play a significant role in the evolutionof the average mass-density structure of massive early-type galaxiesover the past 6 Gyr. We also consider an alternative non-evolutionaryhypothesis based on variations in the strong-lensing measurementaperture with redshift, which would imply the detection of an&quot;inflection zone&quot; marking the transition between the baryon-dominatedand dark-matter halo-dominated regions of the lens galaxies. Furtherobservations of the combined SLACS+BELLS sample can constrain thispicture more precisely, and enable a more detailed investigation of themultivariate dependences of galaxy mass structure across cosmic time.Based on observations made with the NASA/ESA Hubble Space Telescope,obtained at the Space Telescope Science Institute, which is operated bythe Association of Universities for Research in Astronomy, Inc., underNASA contract NAS 5-26555. These observations are associated withprograms 10174, 10494, 10587, 10798, 10886, and 12209.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1201.2988</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Lee, Khee-Gan</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Bartsch, Leslie E.</style></author><author><style face="normal" font="default" size="100%">Carithers, William</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">Margala, Daniel</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Yeche, Christophe</style></author><author><style face="normal" font="default" size="100%">Aubourg, Eric</style></author><author><style face="normal" font="default" size="100%">Bautista, Julian</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blomqvist, Michael</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Borde, Arnaud</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Busca, Nicolas G.</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">Delubac, Timothee</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Ge, Jian</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Le Goff, Jean-Marc</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Miralda-Escude, Jordi</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Noterdaeme, Pasquier</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Paris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Rollinde, Emmanuel</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Rossi, Graziano</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Slosar, Anze</style></author><author><style face="normal" font="default" size="100%">Spergel, David N.</style></author><author><style face="normal" font="default" size="100%">Suzuki, Nao</style></author><author><style face="normal" font="default" size="100%">Viel, Matteo</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The BOSS Lyman-alpha Forest Sample from SDSS Data Release 9</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012arXiv1211.5146L</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1211</style></volume><pages><style face="normal" font="default" size="100%">5146</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present the BOSS Lyman-alpha (Lya) Forest Sample from SDSS DataRelease 9, comprising 54,468 quasar spectra with zqso &gt; 2.15 suitablefor Lya forest analysis. This data set probes the intergalactic mediumwith absorption redshifts 2.0 &lt; z_alpha &lt; 5.7 over an area of 3275square degrees, and encompasses an approximate comoving volume of 20h^-3 Gpc^3. With each spectrum, we have included several productsdesigned to aid in Lya forest analysis: improved sky masks that flagpixels where data may be unreliable, corrections for known biases in thepipeline estimated noise, masks for the cores of damped Lya systems andcorrections for their wings, and estimates of the unabsorbed continua sothat the observed flux can be converted to a fractional transmission.The continua are derived using a principal component fit to the quasarspectrum redwards of restframe Lya (lambda &gt; 1216 Ang), extrapolatedinto the forest region and normalized by a linear function to fit theexpected evolution of the Lya forest mean-flux. The estimated continuum</style></abstract><notes><style face="normal" font="default" size="100%">15 pages, 11 figures; Submitted to AJ</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1211.5146</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Anderson, Lauren</style></author><author><style face="normal" font="default" size="100%">Aubourg, Eric</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Burden, Angela</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz A. N.</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">de Putter, Roland</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Harding, Paul</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Kneib, Jean-Paul</style></author><author><style face="normal" font="default" size="100%">Labatie, Antoine</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">Mehta, Kushal T.</style></author><author><style face="normal" font="default" size="100%">Mena, Olga</style></author><author><style face="normal" font="default" size="100%">Montesano, Francesco</style></author><author><style face="normal" font="default" size="100%">Muna, Demetri</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nuza, Sebastián E.</style></author><author><style face="normal" font="default" size="100%">Olmstead, Matthew D.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Parejko, John</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Reid, Beth</style></author><author><style face="normal" font="default" size="100%">Roe, Natalie A.</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scóccola, Claudia G.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin S.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin A.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, Mariana</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Wagner, Christian</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Yèche, Christophe</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Release 9 spectroscopic galaxy sample</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmological parameters;  cosmology: observations;  dark energy;  distance scale;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.427.3435A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">427</style></volume><pages><style face="normal" font="default" size="100%">3435-3467</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present measurements of galaxy clustering from the Baryon OscillationSpectroscopic Survey (BOSS), which is part of the Sloan Digital SkySurvey III (SDSS-III). These use the Data Release 9 (DR9) CMASS sample,which contains 264 283 massive galaxies covering 3275 square degreeswith an effective redshift z = 0.57 and redshift range 0.43 &lt; z &lt;0.7. Assuming a concordance ΛCDM cosmological model, this samplecovers an effective volume of 2.2 Gpc&lt;SUP&gt;3&lt;/SUP&gt;, and represents thelargest sample of the Universe ever surveyed at this density,n¯≈3×10&lt;SUP&gt;-4&lt;/SUP&gt; h&lt;SUP&gt;-3&lt;/SUP&gt; Mpc 3. We measure theangle-averaged galaxy correlation function and power spectrum, includingdensity-field reconstruction of the baryon acoustic oscillation (BAO)feature. The acoustic features are detected at a significance of5σ in both the correlation function and power spectrum. Combiningwith the SDSS-II luminous red galaxy sample, the detection significanceincreases to 6.7σ. Fitting for the position of the acousticfeatures measures the distance to z = 0.57 relative to the sound horizonD&lt;SUB&gt;V&lt;/SUB&gt;/r&lt;SUB&gt;s&lt;/SUB&gt; = 13.67 ± 0.22 at z = 0.57. Assuminga fiducial sound horizon of 153.19 Mpc, which matches cosmic microwavebackground constraints, this corresponds to a distance D&lt;SUB&gt;V&lt;/SUB&gt; (z= 0.57) = 2094 ± 34 Mpc. At 1.7 per cent, this is the mostprecise distance constraint ever obtained from a galaxy survey. We placethis result alongside previous BAO measurements in a cosmologicaldistance ladder and find excellent agreement with the current supernovameasurements. We use these distance measurements to constrain variouscosmological models, finding continuing support for a flat Universe witha cosmological constant.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1203.6594</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zheng, Zheng</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Chen, Yanmei</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">Nuza, Sebastian E.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Parejko, John K.</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">Sanchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin A.</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Bundy, Kevin</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz N. A.</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Rossi, Graziano</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Streblyanska, Alina</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Luminosity and Color Dependence and Redshift Evolution</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012arXiv1212.1211G</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1212</style></volume><pages><style face="normal" font="default" size="100%">1211</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We measure the luminosity and color dependence and the redshiftevolution of galaxy clustering in the Sloan Digital Sky Survey-IIIBaryon Oscillation Spectroscopic Survey Ninth Data Release. We focus onthe projected two-point correlation function (2PCF) of subsets of itsCMASS sample, which includes about 260,000 galaxies over ~3,300 sq. degin the redshift range 0.43&lt;z&lt;0.7. To minimize the selection effecton galaxy clustering, we construct well-defined luminosity and colorsubsamples by carefully accounting for the CMASS galaxy selection cuts.The 2PCF of the whole CMASS sample, if approximated by a power-law, hasa correlation length of r_0=7.93\pm0.06Mpc/h and an index of\gamma=1.85\pm0.01. Clear dependences on galaxy luminosity and color arefound for the projected 2PCF in all redshift bins, with more luminousand redder galaxies generally exhibiting stronger clustering and steeper2PCF. The color dependence is also clearly seen for galaxies within thered sequence, consistent with the behavior of SDSS-II main samplegalaxies at lower redshifts. At a given luminosity (k+e corrected), nosignificant evolution of the projected 2PCFs with redshift is detectedfor red sequence galaxies. We also construct galaxy samples of fixednumber density at different redshifts, using redshift-dependentmagnitude thresholds. The clustering of these galaxies in the CMASSredshift range is found to be consistent with that predicted by passiveevolution. Our measurements of the luminosity and color dependence andredshift evolution of galaxy clustering will allow for detailed modelingof the relation between galaxies and dark matter halos and newconstraints on galaxy formation and evolution.</style></abstract><notes><style face="normal" font="default" size="100%">21 pages, 17 figures. Submitted to ApJ. Comments Welcome</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1212.1211</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Reid, Beth</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring structure growth using passive galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">surveys;  Cosmology: observations;  dark energy;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.424.2339T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">424</style></volume><pages><style face="normal" font="default" size="100%">2339-2344</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We explore the benefits of using a passively evolving population ofgalaxies to measure the evolution of the rate of structure growthbetween z = 0.25 and 0.65 by combining data from the Sloan Digital SkySurvey (SDSS) I/II and SDSS-III surveys. The large-scale linear bias ofa population of dynamically passive galaxies, which we select from bothsurveys, is easily modelled. Knowing the bias evolution breaksdegeneracies inherent to other methodologies, and decreases theuncertainty in measurements of the rate of structure growth and thenormalization of the galaxy power spectrum by up to a factor of 2. If wetranslate our measurements into a constraint on σ&lt;SUB&gt;8&lt;/SUB&gt;(z =0) assuming a concordance cosmological model and general relativity(GR), we find that using a bias model improves our uncertainty by afactor of nearly 1.5. Our results are consistent with a flat Λcold dark matter model and with GR.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1203.6565</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Reid, Beth</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Montesano, Francesco</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Dorta, Antonio Montero</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, Mariana</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Parejko, John</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: analysis of potential systematics</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmology: observations;  distance scale;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.424..564R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">424</style></volume><pages><style face="normal" font="default" size="100%">564-590</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We analyse the density field of galaxies observed by the Sloan DigitalSky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS)included in the SDSS Data Release Nine (DR9). DR9 includes spectroscopicredshifts for over 400 000 galaxies spread over a footprint of 3275deg&lt;SUP&gt;2&lt;/SUP&gt;. We identify, characterize and mitigate the impact ofsources of systematic uncertainty on large-scale clusteringmeasurements, both for angular moments of the redshift-space correlationfunction, ξ&lt;SUB&gt;ℓ&lt;/SUB&gt;(s), and the spherically averaged powerspectrum, P(k), in order to ensure that robust cosmological constraintswill be obtained from these data. A correlation between the projecteddensity of stars and the higher redshift (0.43 &lt; z &lt; 0.7) galaxysample (the approximately constant stellar mass threshold 'CMASS'sample) due to imaging systematics imparts a systematic error that islarger than the statistical error of the clustering measurements atscales s &gt; 120 h&lt;SUP&gt;-1&lt;/SUP&gt; Mpc or k &lt; 0.01 h Mpc&lt;SUP&gt;-1&lt;/SUP&gt;.We find that these errors can be ameliorated by weighting galaxies basedon their surface brightness and the local stellar density. Theclustering of CMASS galaxies found in the Northern and Southern Galacticfootprints of the survey generally agrees to within 2σ. We usemock galaxy catalogues that simulate the CMASS selection function todetermine that randomly selecting galaxy redshifts in order to simulatethe radial selection function of a random sample imparts the leastsystematic error on ξ&lt;SUB&gt;ℓ&lt;/SUB&gt;(s) measurements and that thissystematic error is negligible for the spherically averaged correlationfunction, ξ&lt;SUB&gt;0&lt;/SUB&gt;. We find a peak in ξ&lt;SUB&gt;0&lt;/SUB&gt; ats˜ 200 h&lt;SUP&gt;-1&lt;/SUP&gt; Mpc, with a corresponding feature withperiod ˜0.03 h Mpc&lt;SUP&gt;-1&lt;/SUP&gt; in P(k), and find features atleast as strong in 4.8 per cent of the mock galaxy catalogues,concluding this feature is likely to be a consequence of cosmicvariance. The methods we recommend for the calculation of clusteringmeasurements using the CMASS sample are adopted in companion papers thatlocate the position of the baryon acoustic oscillation feature,constrain cosmological models using the full shape of ξ&lt;SUB&gt;0&lt;/SUB&gt;and measure the rate of structure growth.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1203.6499</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Reid, Beth A.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">de Putter, Roland</style></author><author><style face="normal" font="default" size="100%">Roe, N. A.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin S.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin A.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z = 0.57 from anisotropic clustering</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">galaxies: haloes;  galaxies: statistics;  cosmological parameters;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.426.2719R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">426</style></volume><pages><style face="normal" font="default" size="100%">2719-2737</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We analyse the anisotropic clustering of massive galaxies from the SloanDigital Sky Survey III Baryon Oscillation Spectroscopic Survey (BOSS)Data Release 9 (DR9) sample, which consists of 264 283 galaxies in theredshift range 0.43 &lt; z &lt; 0.7 spanning 3275 deg&lt;SUP&gt;2&lt;/SUP&gt;. Bothpeculiar velocities and errors in the assumed redshift-distance relation('Alcock-Paczynski effect') generate correlations between clusteringamplitude and orientation with respect to the line of sight. Togetherwith the sharp baryon acoustic oscillation (BAO) standard ruler, ourmeasurements of the broad-band shape of the monopole and quadrupolecorrelation functions simultaneously constrain the comoving angulardiameter distance (2190 ± 61 Mpc) to z = 0.57, the Hubbleexpansion rate at z = 0.57 (92.4 ± 4.5 km s&lt;SUP&gt;-1&lt;/SUP&gt;Mpc&lt;SUP&gt;-1&lt;/SUP&gt;) and the growth rate of structure at that same redshift(dσ&lt;SUB&gt;8&lt;/SUB&gt;/d ln a = 0.43 ± 0.069). Our analysisprovides the best current direct determination of both D&lt;SUB&gt;A&lt;/SUB&gt; andH in galaxy clustering data using this technique. If we further assume aΛcold dark matter expansion history, our growth constrainttightens to dσ&lt;SUB&gt;8&lt;/SUB&gt;/d ln a = 0.415 ± 0.034. Incombination with the cosmic microwave background, our measurements ofD&lt;SUB&gt;A&lt;/SUB&gt;, H and dσ&lt;SUB&gt;8&lt;/SUB&gt;/d ln a all separately requiredark energy at z &gt; 0.57, and when combined implyΩ&lt;SUB&gt;Λ&lt;/SUB&gt; = 0.74 ± 0.016, independent of theUniverse's evolution at z &lt; 0.57. All of these constraints assumescale-independent linear growth, and assume general relativity tocompute both O(10 per cent) non-linear model corrections and our errors.In our companion paper, Samushia et al., we explore further cosmologicalimplications of these observations.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1203.6641</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Scóccola, C. G.</style></author><author><style face="normal" font="default" size="100%">Ross, A. J.</style></author><author><style face="normal" font="default" size="100%">Percival, W.</style></author><author><style face="normal" font="default" size="100%">Manera, M.</style></author><author><style face="normal" font="default" size="100%">Montesano, F.</style></author><author><style face="normal" font="default" size="100%">Mazzalay, X.</style></author><author><style face="normal" font="default" size="100%">Cuesta, A. J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Kazin, E.</style></author><author><style face="normal" font="default" size="100%">McBride, C. K.</style></author><author><style face="normal" font="default" size="100%">Mehta, K.</style></author><author><style face="normal" font="default" size="100%">Montero-Dorta, A. D.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, N.</style></author><author><style face="normal" font="default" size="100%">Prada, F.</style></author><author><style face="normal" font="default" size="100%">Rubiño-Martín, J. A.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, R.</style></author><author><style face="normal" font="default" size="100%">Xu, X.</style></author><author><style face="normal" font="default" size="100%">Magaña, M. Vargas</style></author><author><style face="normal" font="default" size="100%">Aubourg, E.</style></author><author><style face="normal" font="default" size="100%">Bahcall, N. A.</style></author><author><style face="normal" font="default" size="100%">Bailey, S.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, D.</style></author><author><style face="normal" font="default" size="100%">Bolton, A. S.</style></author><author><style face="normal" font="default" size="100%">Brewington, H.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, J. R.</style></author><author><style face="normal" font="default" size="100%">Gott, J. Richard</style></author><author><style face="normal" font="default" size="100%">Hamilton, J. C.</style></author><author><style face="normal" font="default" size="100%">Ho, S.</style></author><author><style face="normal" font="default" size="100%">Honscheid, K.</style></author><author><style face="normal" font="default" size="100%">Labatie, A.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, E.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, V.</style></author><author><style face="normal" font="default" size="100%">Maraston, C.</style></author><author><style face="normal" font="default" size="100%">Muna, D.</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Oravetz, D.</style></author><author><style face="normal" font="default" size="100%">Pan, K.</style></author><author><style face="normal" font="default" size="100%">Ross, N. P.</style></author><author><style face="normal" font="default" size="100%">Roe, N. A.</style></author><author><style face="normal" font="default" size="100%">Reid, B. A.</style></author><author><style face="normal" font="default" size="100%">Schlegel, D. J.</style></author><author><style face="normal" font="default" size="100%">Shelden, A.</style></author><author><style face="normal" font="default" size="100%">Schneider, D. P.</style></author><author><style face="normal" font="default" size="100%">Simmons, A.</style></author><author><style face="normal" font="default" size="100%">Skibba, R.</style></author><author><style face="normal" font="default" size="100%">Snedden, S.</style></author><author><style face="normal" font="default" size="100%">Thomas, D.</style></author><author><style face="normal" font="default" size="100%">Tinker, J.</style></author><author><style face="normal" font="default" size="100%">Wake, D. A.</style></author><author><style face="normal" font="default" size="100%">Weaver, B. A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Zehavi, I.</style></author><author><style face="normal" font="default" size="100%">Zhao, G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large-scale two-point correlation function</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmological parameters;  large-scale structure of Universe</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012MNRAS.425..415S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">425</style></volume><pages><style face="normal" font="default" size="100%">415-437</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We obtain constraints on cosmological parameters from the sphericallyaveraged redshift-space correlation function of the CMASS Data Release 9(DR9) sample of the Baryonic Oscillation Spectroscopic Survey (BOSS). Wecombine this information with additional data from recent cosmicmicrowave background (CMB), supernova and baryon acoustic oscillationmeasurements. Our results show no significant evidence of deviationsfrom the standard flat Λ cold dark matter model, whose basicparameters can be specified by Ω&lt;SUB&gt;m&lt;/SUB&gt; = 0.285 ±0.009, 100 Ω&lt;SUB&gt;b&lt;/SUB&gt; = 4.59 ± 0.09, n&lt;SUB&gt;s&lt;/SUB&gt; =0.961 ± 0.009, H&lt;SUB&gt;0&lt;/SUB&gt; = 69.4 ± 0.8 kms&lt;SUP&gt;-1&lt;/SUP&gt; Mpc&lt;SUP&gt;-1&lt;/SUP&gt; and σ&lt;SUB&gt;8&lt;/SUB&gt; = 0.80 ±0.02. The CMB+CMASS combination sets tight constraints on the curvatureof the Universe, with Ω&lt;SUB&gt;k&lt;/SUB&gt; = -0.0043 ± 0.0049, andthe tensor-to-scalar amplitude ratio, for which we find r &lt; 0.16 atthe 95 per cent confidence level (CL). These data show a clear signatureof a deviation from scale invariance also in the presence of tensormodes, with n&lt;SUB&gt;s&lt;/SUB&gt; &lt; 1 at the 99.7 per cent CL. We deriveconstraints on the fraction of massive neutrinos of f&lt;SUB&gt;ν&lt;/SUB&gt;&lt; 0.049 (95 per cent CL), implying a limit of ∑m&lt;SUB&gt;ν&lt;/SUB&gt;&lt; 0.51 eV. We find no signature of a deviation from a cosmologicalconstant from the combination of all data sets, with a constraint ofw&lt;SUB&gt;DE&lt;/SUB&gt; = -1.033 ± 0.073 when this parameter is assumedtime-independent, and no evidence of a departure from this value when itis allowed to evolve as w&lt;SUB&gt;DE&lt;/SUB&gt;(a) = w&lt;SUB&gt;0&lt;/SUB&gt; +w&lt;SUB&gt;a&lt;/SUB&gt;(1 - a). The achieved accuracy on our cosmologicalconstraints is a clear demonstration of the constraining power ofcurrent cosmological observations.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1203.6616</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">de Putter, Roland</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Saito, Shun</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schlafly, Eddie</style></author><author><style face="normal" font="default" size="100%">Seljak, Uros</style></author><author><style face="normal" font="default" size="100%">Hernández-Monteagudo, Carlos</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin</style></author><author><style face="normal" font="default" size="100%">Schneider, Don</style></author><author><style face="normal" font="default" size="100%">Reid, Beth</style></author><author><style face="normal" font="default" size="100%">Mena, Olga</style></author><author><style face="normal" font="default" size="100%">Viel, Matteo</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dimitry</style></author><author><style face="normal" font="default" size="100%">Brewinton, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkman, Jon</style></author><author><style face="normal" font="default" size="100%">Nicolaci da Costa, Luiz</style></author><author><style face="normal" font="default" size="100%">Gott, John R.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Nichol, Bob</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">de Simoni, Fernando</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Yeche, Christophe</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Clustering of Sloan Digital Sky Survey III Photometric Luminous Galaxies: The Measurement, Systematics, and Cosmological Implications</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmological parameters;  dark energy;  dark matter;  distance scale</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...761...14H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">761</style></volume><pages><style face="normal" font="default" size="100%">14</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey (SDSS) surveyed 14,555 deg&lt;SUP&gt;2&lt;/SUP&gt;, anddelivered over a trillion pixels of imaging data. We present a study ofgalaxy clustering using 900,000 luminous galaxies with photometricredshifts, spanning between z = 0.45 and z = 0.65, constructed from theSDSS using methods described in Ross et al. This data set spans 11,000deg&lt;SUP&gt;2&lt;/SUP&gt; and probes a volume of 3 h &lt;SUP&gt;-3&lt;/SUP&gt;Gpc&lt;SUP&gt;3&lt;/SUP&gt;, making it the largest volume ever used for galaxyclustering measurements. We describe in detail the construction of thesurvey window function and various systematics affecting ourmeasurement. With such a large volume, high-precision cosmologicalconstraints can be obtained given careful control and understanding ofthe observational systematics. We present a novel treatment of theobservational systematics and its applications to the clustering signalsfrom the data set. In this paper, we measure the angular clusteringusing an optimal quadratic estimator at four redshift slices with an</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1201.2137</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hand, Nick</style></author><author><style face="normal" font="default" size="100%">Addison, Graeme E.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Eric</style></author><author><style face="normal" font="default" size="100%">Battaglia, Nick</style></author><author><style face="normal" font="default" size="100%">Battistelli, Elia S.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Bond, J. Richard</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Brown, Benjamin R.</style></author><author><style face="normal" font="default" size="100%">Das, Sudeep</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">Devlin, Mark J.</style></author><author><style face="normal" font="default" size="100%">Dunkley, Joanna</style></author><author><style face="normal" font="default" size="100%">Dunner, Rolando</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Fowler, Joseph W.</style></author><author><style face="normal" font="default" size="100%">Gralla, Megan B.</style></author><author><style face="normal" font="default" size="100%">Hajian, Amir</style></author><author><style face="normal" font="default" size="100%">Halpern, Mark</style></author><author><style face="normal" font="default" size="100%">Hilton, Matt</style></author><author><style face="normal" font="default" size="100%">Hincks, Adam D.</style></author><author><style face="normal" font="default" size="100%">Hlozek, Renée</style></author><author><style face="normal" font="default" size="100%">Hughes, John P.</style></author><author><style face="normal" font="default" size="100%">Infante, Leopoldo</style></author><author><style face="normal" font="default" size="100%">Irwin, Kent D.</style></author><author><style face="normal" font="default" size="100%">Kosowsky, Arthur</style></author><author><style face="normal" font="default" size="100%">Lin, Yen-Ting</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Marriage, Tobias A.</style></author><author><style face="normal" font="default" size="100%">Marsden, Danica</style></author><author><style face="normal" font="default" size="100%">Menanteau, Felipe</style></author><author><style face="normal" font="default" size="100%">Moodley, Kavilan</style></author><author><style face="normal" font="default" size="100%">Niemack, Michael D.</style></author><author><style face="normal" font="default" size="100%">Nolta, Michael R.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Page, Lyman A.</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Reese, Erik D.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Sehgal, Neelima</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Sievers, Jon</style></author><author><style face="normal" font="default" size="100%">Sifón, Cristóbal</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie</style></author><author><style face="normal" font="default" size="100%">Spergel, David N.</style></author><author><style face="normal" font="default" size="100%">Staggs, Suzanne T.</style></author><author><style face="normal" font="default" size="100%">Swetz, Daniel S.</style></author><author><style face="normal" font="default" size="100%">Switzer, Eric R.</style></author><author><style face="normal" font="default" size="100%">Trac, Hy</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Wollack, Edward J.</style></author><author><style face="normal" font="default" size="100%">Yeche, Christophe</style></author><author><style face="normal" font="default" size="100%">Zunckel, Caroline</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Evidence of Galaxy Cluster Motions with the Kinematic Sunyaev-Zel'dovich Effect</style></title><secondary-title><style face="normal" font="default" size="100%">Physical Review Letters</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Observational cosmology;  Distances;  redshifts;  radial velocities; spatial distribution of galaxies;  Galaxy clusters;  Background radiations</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012PhRvL.109d1101H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">109</style></volume><pages><style face="normal" font="default" size="100%">41101</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Using high-resolution microwave sky maps made by the Atacama CosmologyTelescope, we for the first time present strong evidence for motions ofgalaxy clusters and groups via microwave background temperaturedistortions due to the kinematic Sunyaev-Zel’dovich effect. Galaxyclusters are identified by their constituent luminous galaxies observedby the Baryon Oscillation Spectroscopic Survey, part of the SloanDigital Sky Survey III. We measure the mean pairwise momentum ofclusters, with a probability of the signal being due to random errors of0.002, and the signal is consistent with the growth of cosmic structurein the standard model of cosmology.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1203.4219</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Caldwell, Nelson</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Forman, William R.</style></author><author><style face="normal" font="default" size="100%">Hickox, Ryan C.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Jones, Christine</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Murray, Stephen S.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Galaxy Optical Luminosity Function from the AGN and Galaxy Evolution Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">galaxies: luminosity function;  mass function;  galaxies: statistics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...748...10C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">748</style></volume><pages><style face="normal" font="default" size="100%">10</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present the galaxy optical luminosity function for the redshift range0.05 &lt; z &lt; 0.75 from the AGN and Galaxy Evolution Survey, aspectroscopic survey of 7.6 deg&lt;SUP&gt;2&lt;/SUP&gt; in the Boötes field ofthe NOAO Deep Wide-Field Survey. Our statistical sample is composed of12,473 galaxies with known redshifts down to I = 20.4 (AB). Our resultsat low redshift are consistent with those from Sloan Digital Sky Survey;at higher redshift, we find strong evidence for evolution in theluminosity function, including differential evolution between blue andred galaxies. We find that the luminosity density evolves as (1 +z)&lt;SUP&gt;(0.54 ± 0.64)&lt;/SUP&gt; for red galaxies and (1 + z)&lt;SUP&gt;(1.64± 0.39)&lt;/SUP&gt; for blue galaxies.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1201.2954</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Measuring D_A and H at z=0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012arXiv1206.6732X</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1206</style></volume><pages><style face="normal" font="default" size="100%">6732</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present measurements of the angular diameter distance D_A(z) and theHubble parameter H(z) at z=0.35 using the anisotropy of the baryonacoustic oscillation (BAO) signal measured in the galaxy clusteringdistribution of the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7)Luminous Red Galaxies (LRG) sample. Our work is the first to applydensity-field reconstruction to an anisotropic analysis of the acousticpeak. Reconstruction partially removes the effects of non-linearevolution and redshift-space distortions in order to sharpen theacoustic signal. We present the theoretical framework behind theanisotropic BAO signal and give a detailed account of the fitting modelwe use to extract this signal from the data. Our method focuses only onthe acoustic peak anisotropy, rather than the more model-dependentanisotropic information from the broadband power. We test the robustnessof our analysis methods on 160 LasDamas DR7 mock catalogues and find</style></abstract><notes><style face="normal" font="default" size="100%">29 pages, 21 figures, submitted to MNRAS</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1206.6732</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz N.</style></author><author><style face="normal" font="default" size="100%">Cunha, Katia</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett L.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, Peter M.</style></author><author><style face="normal" font="default" size="100%">Elia García Pérez, Ana</style></author><author><style face="normal" font="default" size="100%">Girardi, Léo</style></author><author><style face="normal" font="default" size="100%">Hearty, Fred R.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio A. G.</style></author><author><style face="normal" font="default" size="100%">Majewski, Steven R.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Mészáros, Szabolcs</style></author><author><style face="normal" font="default" size="100%">Nidever, David L.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Robert W.</style></author><author><style face="normal" font="default" size="100%">O'Donnell, Christine</style></author><author><style face="normal" font="default" size="100%">Oravetz, Audrey</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Rocha-Pinto, Helio J.</style></author><author><style face="normal" font="default" size="100%">Schiavon, Ricardo P.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schultheis, Mathias</style></author><author><style face="normal" font="default" size="100%">Skrutskie, Michael</style></author><author><style face="normal" font="default" size="100%">Smith, Verne V.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Wilson, John C.</style></author><author><style face="normal" font="default" size="100%">Zasowski, Gail</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Milky Way's Circular-velocity Curve between 4 and 14 kpc from APOGEE data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Galaxy: disk;  Galaxy: fundamental parameters;  Galaxy: general;  Galaxy: kinematics and dynamics;  Galaxy: structure;  stars: kinematics and dynamics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...759..131B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">759</style></volume><pages><style face="normal" font="default" size="100%">131</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We measure the Milky Way's rotation curve over the Galactocentric range4 kpc &lt;~ R &lt;~ 14 kpc from the first year of data from the ApachePoint Observatory Galactic Evolution Experiment. We model theline-of-sight velocities of 3365 stars in 14 fields with b = 0°between 30° &lt;= l &lt;= 210° out to distances of 10 kpc usingan axisymmetric kinematical model that includes a correction for theasymmetric drift of the warm tracer population (σ&lt;SUB&gt; R &lt;/SUB&gt;≈ 35 km s&lt;SUP&gt;-1&lt;/SUP&gt;). We determine the local value of thecircular velocity to be V&lt;SUB&gt;c&lt;/SUB&gt; (R &lt;SUB&gt;0&lt;/SUB&gt;) = 218 ± 6km s&lt;SUP&gt;-1&lt;/SUP&gt; and find that the rotation curve isapproximately flat with a local derivative between -3.0 kms&lt;SUP&gt;-1&lt;/SUP&gt; kpc&lt;SUP&gt;-1&lt;/SUP&gt; and 0.4 kms&lt;SUP&gt;-1&lt;/SUP&gt; kpc&lt;SUP&gt;-1&lt;/SUP&gt;. We also measure the Sun'sposition and velocity in the Galactocentric rest frame, finding thedistance to the Galactic center to be 8 kpc &lt; R &lt;SUB&gt;0&lt;/SUB&gt; &lt; 9kpc, radial velocity V &lt;SUB&gt; R, &amp;sun;&lt;/SUB&gt; = -10 ± 1 kms&lt;SUP&gt;-1&lt;/SUP&gt;, and rotational velocity V &lt;SUB&gt;phi, &amp;sun;&lt;/SUB&gt;= 242&lt;SUP&gt;+10&lt;/SUP&gt; &lt;SUB&gt;- 3&lt;/SUB&gt; km s&lt;SUP&gt;-1&lt;/SUP&gt;, ingood agreement with local measurements of the Sun's radial velocity andwith the observed proper motion of Sgr A*. We investigate varioussystematic uncertainties and find that these are limited to offsets atthe percent level, ~2 km s&lt;SUP&gt;-1&lt;/SUP&gt; in V&lt;SUB&gt;c&lt;/SUB&gt; .Marginalizing over all the systematics that we consider, we find thatV&lt;SUB&gt;c&lt;/SUB&gt; (R &lt;SUB&gt;0&lt;/SUB&gt;) &lt; 235 km s&lt;SUP&gt;-1&lt;/SUP&gt; at</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1209.0759</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ahn, Christopher P.</style></author><author><style face="normal" font="default" size="100%">Alexandroff, Rachael</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Anderton, Timothy</style></author><author><style face="normal" font="default" size="100%">Andrews, Brett H.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Balbinot, Eduardo</style></author><author><style face="normal" font="default" size="100%">Barnes, Rory</style></author><author><style face="normal" font="default" size="100%">Bautista, Julian</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Beifiori, Alessandra</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bhardwaj, Vaishali</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blake, Cullen H.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Blomqvist, Michael</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Borde, Arnaud</style></author><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brown, Peter J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Bundy, Kevin</style></author><author><style face="normal" font="default" size="100%">Busca, N. G.</style></author><author><style face="normal" font="default" size="100%">Carithers, William</style></author><author><style face="normal" font="default" size="100%">Carnero, Aurelio R.</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Casetti-Dinescu, Dana I.</style></author><author><style face="normal" font="default" size="100%">Chen, Yanmei</style></author><author><style face="normal" font="default" size="100%">Chiappini, Cristina</style></author><author><style face="normal" font="default" size="100%">Comparat, Johan</style></author><author><style face="normal" font="default" size="100%">Connolly, Natalia</style></author><author><style face="normal" font="default" size="100%">Crepp, Justin R.</style></author><author><style face="normal" font="default" size="100%">Cristiani, Stefano</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz N.</style></author><author><style face="normal" font="default" size="100%">Davenport, James R. A.</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">de Putter, Roland</style></author><author><style face="normal" font="default" size="100%">De Lee, Nathan</style></author><author><style face="normal" font="default" size="100%">Delubac, Timothée</style></author><author><style face="normal" font="default" size="100%">Dhital, Saurav</style></author><author><style face="normal" font="default" size="100%">Ealet, Anne</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett L.</style></author><author><style face="normal" font="default" size="100%">Edmondson, Edward M.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Escoffier, S.</style></author><author><style face="normal" font="default" size="100%">Esposito, Massimiliano</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Femenía Castellá, Bruno</style></author><author><style face="normal" font="default" size="100%">Fernández Alvar, Emma</style></author><author><style face="normal" font="default" size="100%">Ferreira, Leticia D.</style></author><author><style face="normal" font="default" size="100%">Filiz Ak, N.</style></author><author><style face="normal" font="default" size="100%">Finley, Hayley</style></author><author><style face="normal" font="default" size="100%">Fleming, Scott W.</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, Peter M.</style></author><author><style face="normal" font="default" size="100%">García-Hernández, D. A.</style></author><author><style face="normal" font="default" size="100%">García Pérez, A. E.</style></author><author><style face="normal" font="default" size="100%">Ge, Jian</style></author><author><style face="normal" font="default" size="100%">Génova-Santos, R.</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce A.</style></author><author><style face="normal" font="default" size="100%">Girardi, Léo</style></author><author><style face="normal" font="default" size="100%">González Hernández, Jonay I.</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Guo, Hong</style></author><author><style face="normal" font="default" size="100%">Haggard, Daryl</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Harris, David W.</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hearty, Frederick R.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Huehnerhoff, J.</style></author><author><style face="normal" font="default" size="100%">Ivans, Inese I.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jacobson, Heather R.</style></author><author><style face="normal" font="default" size="100%">Jiang, Linhua</style></author><author><style face="normal" font="default" size="100%">Johansson, Jonas</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Kauffmann, Guinevere</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Kirkpatrick, Jessica A.</style></author><author><style face="normal" font="default" size="100%">Klaene, Mark A.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kneib, Jean-Paul</style></author><author><style face="normal" font="default" size="100%">Le Goff, Jean-Marc</style></author><author><style face="normal" font="default" size="100%">Leauthaud, Alexie</style></author><author><style face="normal" font="default" size="100%">Lee, Khee-Gan</style></author><author><style face="normal" font="default" size="100%">Lee, Young Sun</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Lucatello, Sara</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Ma, Bo</style></author><author><style face="normal" font="default" size="100%">Ma, Zhibo</style></author><author><style face="normal" font="default" size="100%">MacDonald, Nicholas</style></author><author><style face="normal" font="default" size="100%">Mack, Claude E.</style></author><author><style face="normal" font="default" size="100%">Mahadevan, Suvrath</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio A. G.</style></author><author><style face="normal" font="default" size="100%">Majewski, Steven R.</style></author><author><style face="normal" font="default" size="100%">Makler, Martin</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Manchado, A.</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Manera, Marc</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Margala, Daniel</style></author><author><style face="normal" font="default" size="100%">Martell, Sarah L.</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">McGreer, Ian D.</style></author><author><style face="normal" font="default" size="100%">McMahon, Richard G.</style></author><author><style face="normal" font="default" size="100%">Ménard, Brice</style></author><author><style face="normal" font="default" size="100%">Meszaros, Sz.</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, Jordi</style></author><author><style face="normal" font="default" size="100%">Montero-Dorta, Antonio D.</style></author><author><style face="normal" font="default" size="100%">Montesano, Francesco</style></author><author><style face="normal" font="default" size="100%">Morrison, Heather L.</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Murayama, Hitoshi</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Neto, A. F.</style></author><author><style face="normal" font="default" size="100%">Cuong Nguyen, Duy</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nidever, David L.</style></author><author><style face="normal" font="default" size="100%">Noterdaeme, Pasquier</style></author><author><style face="normal" font="default" size="100%">Nuza, Sebastián E.</style></author><author><style face="normal" font="default" size="100%">Ogando, Ricardo L. C.</style></author><author><style face="normal" font="default" size="100%">Olmstead, Matthew D.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Parejko, John K.</style></author><author><style face="normal" font="default" size="100%">Parihar, Prachi</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Pattarakijwanich, Petchara</style></author><author><style face="normal" font="default" size="100%">Pepper, Joshua</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Pérez-Fournon, Ismael</style></author><author><style face="normal" font="default" size="100%">Pérez-Ràfols, Ignasi</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Pforr, Janine</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Pinsonneault, Marc H.</style></author><author><style face="normal" font="default" size="100%">Porto de Mello, G. F.</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Price-Whelan, Adrian M.</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Rebolo, Rafael</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Robin, Annie C.</style></author><author><style face="normal" font="default" size="100%">Rocha-Pinto, Helio J.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Roe, Natalie A.</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Rossi, Graziano</style></author><author><style face="normal" font="default" size="100%">Rubiño-Martin, J. A.</style></author><author><style face="normal" font="default" size="100%">Samushia, Lado</style></author><author><style face="normal" font="default" size="100%">Sanchez Almeida, J.</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Santiago, Basílio</style></author><author><style face="normal" font="default" size="100%">Sayres, Conor</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schlesinger, Katharine J.</style></author><author><style face="normal" font="default" size="100%">Schmidt, Sarah J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schultheis, Mathias</style></author><author><style face="normal" font="default" size="100%">Schwope, Axel D.</style></author><author><style face="normal" font="default" size="100%">Scóccola, C. G.</style></author><author><style face="normal" font="default" size="100%">Seljak, Uros</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shen, Yue</style></author><author><style face="normal" font="default" size="100%">Shu, Yiping</style></author><author><style face="normal" font="default" size="100%">Simmerer, Jennifer</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey E.</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin A.</style></author><author><style face="normal" font="default" size="100%">Skrutskie, M. F.</style></author><author><style face="normal" font="default" size="100%">Slosar, A.</style></author><author><style face="normal" font="default" size="100%">Sobreira, Flavia</style></author><author><style face="normal" font="default" size="100%">Sobeck, Jennifer S.</style></author><author><style face="normal" font="default" size="100%">Stassun, Keivan G.</style></author><author><style face="normal" font="default" size="100%">Steele, Oliver</style></author><author><style face="normal" font="default" size="100%">Steinmetz, Matthias</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Streblyanska, Alina</style></author><author><style face="normal" font="default" size="100%">Suzuki, Nao</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly E. C.</style></author><author><style face="normal" font="default" size="100%">Tal, Tomer</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Thompson, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, M.</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Viel, Matteo</style></author><author><style face="normal" font="default" size="100%">Vikas, Shailendra K.</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Wang, Ji</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Weiner, Benjamin J.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Wilson, John C.</style></author><author><style face="normal" font="default" size="100%">Wisniewski, John P.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. M.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yèche, Christophe</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zamora, O.</style></author><author><style face="normal" font="default" size="100%">Zasowski, Gail</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zhao, Gong-bo</style></author><author><style face="normal" font="default" size="100%">Zheng, Zheng</style></author><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author><author><style face="normal" font="default" size="100%">Zinn, Joel C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Ninth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">atlases;  catalogs;  surveys</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJS..203...21A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">203</style></volume><pages><style face="normal" font="default" size="100%">21</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey III (SDSS-III) presents the firstspectroscopic data from the Baryon Oscillation Spectroscopic Survey(BOSS). This ninth data release (DR9) of the SDSS project includes535,995 new galaxy spectra (median z ~ 0.52), 102,100 new quasar spectra(median z ~ 2.32), and 90,897 new stellar spectra, along with the datapresented in previous data releases. These spectra were obtained withthe new BOSS spectrograph and were taken between 2009 December and 2011July. In addition, the stellar parameters pipeline, which determinesradial velocities, surface temperatures, surface gravities, andmetallicities of stars, has been updated and refined with improvementsin temperature estimates for stars with T &lt;SUB&gt;eff&lt;/SUB&gt; &lt; 5000 K andin metallicity estimates for stars with [Fe/H] &gt; -0.5. DR9 includesnew stellar parameters for all stars presented in DR8, including starsfrom SDSS-I and II, as well as those observed as part of the SEGUE-2.The astrometry error introduced in the DR8 imaging catalogs has beencorrected in the DR9 data products. The next data release for SDSS-IIIwill be in Summer 2013, which will present the first data from theAPOGEE along with another year of data from BOSS, followed by the finalSDSS-III data release in 2014 December.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1207.7137</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>13</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Mortonson, Michael J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Hirata, Christopher</style></author><author><style face="normal" font="default" size="100%">Riess, Adam G.</style></author><author><style face="normal" font="default" size="100%">Rozo, Eduardo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Observational Probes of Cosmic Acceleration</style></title><secondary-title><style face="normal" font="default" size="100%">ArXiv e-prints</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Cosmology and Extragalactic Astrophysics</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012arXiv1201.2434W</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1201</style></volume><pages><style face="normal" font="default" size="100%">2434</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The accelerating expansion of the universe is the most surprisingcosmological discovery in many decades, implying that the universe isdominated by some form of &quot;dark energy&quot; with exotic physical properties,or that Einstein's theory of gravity breaks down on cosmological scales.The profound implications of cosmic acceleration have inspired ambitiousexperimental efforts to measure the history of expansion and growth ofstructure with percent-level precision or higher. We review in detailthe four most well established methods for making such measurements:Type Ia supernovae, baryon acoustic oscillations (BAO), weakgravitational lensing, and galaxy clusters. We pay particular attentionto the systematic uncertainties in these techniques and to strategiesfor controlling them at the level needed to exploit &quot;Stage IV&quot; darkenergy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We brieflyreview a number of other approaches including redshift-spacedistortions, the Alcock-Paczynski test, and direct measurements of H_0.We present extensive forecasts for constraints on the dark energyequation of state and parameterized deviations from GR, achievable withStage III and Stage IV experimental programs that incorporatesupernovae, BAO, weak lensing, and CMB data. We also show the level ofprecision required for other methods to provide constraints competitivewith those of these fiducial programs. We emphasize the value of abalanced program that employs several of the most powerful methods incombination, both to cross-check systematic uncertainties and to takeadvantage of complementary information. Surveys to probe cosmicacceleration produce data sets with broad applications, and theycontinue the longstanding astronomical tradition of mapping the universein ever greater detail over ever larger scales.</style></abstract><notes><style face="normal" font="default" size="100%">252 pages(!) 49 figures. Review article for Physics Reports. Comments welcome; those received before 2/17/12 will be considered before revised submission</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1201.2434</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>47</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Wilson, John C.</style></author><author><style face="normal" font="default" size="100%">Hearty, F.</style></author><author><style face="normal" font="default" size="100%">Skrutskie, M. F.</style></author><author><style face="normal" font="default" size="100%">Majewski, S. R.</style></author><author><style face="normal" font="default" size="100%">Schiavon, R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Gunn, J.</style></author><author><style face="normal" font="default" size="100%">Holtzman, J.</style></author><author><style face="normal" font="default" size="100%">Nidever, D.</style></author><author><style face="normal" font="default" size="100%">Gillespie, B.</style></author><author><style face="normal" font="default" size="100%">Weinberg, D.</style></author><author><style face="normal" font="default" size="100%">Blank, B.</style></author><author><style face="normal" font="default" size="100%">Henderson, C.</style></author><author><style face="normal" font="default" size="100%">Smee, S.</style></author><author><style face="normal" font="default" size="100%">Barkhouser, R.</style></author><author><style face="normal" font="default" size="100%">Harding, A.</style></author><author><style face="normal" font="default" size="100%">Hope, S.</style></author><author><style face="normal" font="default" size="100%">Fitzgerald, G.</style></author><author><style face="normal" font="default" size="100%">Stolberg, T.</style></author><author><style face="normal" font="default" size="100%">Arns, J.</style></author><author><style face="normal" font="default" size="100%">Nelson, M.</style></author><author><style face="normal" font="default" size="100%">Brunner, S.</style></author><author><style face="normal" font="default" size="100%">A. Burton</style></author><author><style face="normal" font="default" size="100%">E. Walker</style></author><author><style face="normal" font="default" size="100%">Lam, C.</style></author><author><style face="normal" font="default" size="100%">Maseman, P.</style></author><author><style face="normal" font="default" size="100%">Barr, J.</style></author><author><style face="normal" font="default" size="100%">Leger, F.</style></author><author><style face="normal" font="default" size="100%">Carey, L.</style></author><author><style face="normal" font="default" size="100%">MacDonald, N.</style></author><author><style face="normal" font="default" size="100%">Ebelke, G.</style></author><author><style face="normal" font="default" size="100%">Beland, S.</style></author><author><style face="normal" font="default" size="100%">Horne, T.</style></author><author><style face="normal" font="default" size="100%">Young, E.</style></author><author><style face="normal" font="default" size="100%">Rieke, G.</style></author><author><style face="normal" font="default" size="100%">Rieke, M.</style></author><author><style face="normal" font="default" size="100%">O'Brien, T.</style></author><author><style face="normal" font="default" size="100%">Crane, J.</style></author><author><style face="normal" font="default" size="100%">Carr, M.</style></author><author><style face="normal" font="default" size="100%">Harrison, C.</style></author><author><style face="normal" font="default" size="100%">Stoll, R.</style></author><author><style face="normal" font="default" size="100%">Vernieri, M.</style></author><author><style face="normal" font="default" size="100%">Shetrone, M.</style></author><author><style face="normal" font="default" size="100%">Allende-Prieto, C.</style></author><author><style face="normal" font="default" size="100%">Johnson, J.</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, P.</style></author><author><style face="normal" font="default" size="100%">Zasowski, G.</style></author><author><style face="normal" font="default" size="100%">Garcia Perez, A.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, D.</style></author><author><style face="normal" font="default" size="100%">Cunha, K.</style></author><author><style face="normal" font="default" size="100%">Smith, V. V.</style></author><author><style face="normal" font="default" size="100%">Meszaros, Sz.</style></author><author><style face="normal" font="default" size="100%">Zhao, B.</style></author><author><style face="normal" font="default" size="100%">Hayden, M.</style></author><author><style face="normal" font="default" size="100%">Chojnowski, S. D.</style></author><author><style face="normal" font="default" size="100%">Andrews, B.</style></author><author><style face="normal" font="default" size="100%">Loomis, C.</style></author><author><style face="normal" font="default" size="100%">Owen, R.</style></author><author><style face="normal" font="default" size="100%">Klaene, M.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Stauffer, F.</style></author><author><style face="normal" font="default" size="100%">Long, D.</style></author><author><style face="normal" font="default" size="100%">Jordan, W.</style></author><author><style face="normal" font="default" size="100%">Holder, D.</style></author><author><style face="normal" font="default" size="100%">Cope, F.</style></author><author><style face="normal" font="default" size="100%">Naugle, T.</style></author><author><style face="normal" font="default" size="100%">Pfaffenberger, B.</style></author><author><style face="normal" font="default" size="100%">Schlegel, D.</style></author><author><style face="normal" font="default" size="100%">Blanton, M.</style></author><author><style face="normal" font="default" size="100%">Muna, D.</style></author><author><style face="normal" font="default" size="100%">Weaver, B.</style></author><author><style face="normal" font="default" size="100%">Snedden, S.</style></author><author><style face="normal" font="default" size="100%">Pan, K.</style></author><author><style face="normal" font="default" size="100%">Brewington, H.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, E.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, V.</style></author><author><style face="normal" font="default" size="100%">Simmons, A.</style></author><author><style face="normal" font="default" size="100%">Oravetz, D.</style></author><author><style face="normal" font="default" size="100%">Mahadevan, S.</style></author><author><style face="normal" font="default" size="100%">Halverson, S.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Performance of the Apache Point Observatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph</style></title><secondary-title><style face="normal" font="default" size="100%">Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012SPIE.8446E..0HW</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">8446</style></volume><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The Apache Point Observatory Galactic Evolution Experiment (APOGEE) usesa dedicated 300-fiber, narrow-band near-infrared (1.51-1.7 μm), highresolution (R~22,500) spectrograph to survey approximately 100,000 giantstars across the Milky Way. This three-year survey, in operation sincelate-summer 2011 as part of the Sloan Digital Sky Survey III (SDSS III),will revolutionize our understanding of the kinematical and chemicalenrichment histories of all Galactic stellar populations. We present theperformance of the instrument from its first year in operation. Theinstrument is housed in a separate building adjacent to the 2.5-m SDSStelescope and fed light via approximately 45-meter fiber runs from thetelescope. The instrument design includes numerous innovations includinga gang connector that allows simultaneous connection of all fibers witha single plug to a telescope cartridge that positions the fibers on thesky, numerous places in the fiber train in which focal ratio degradationhad to be minimized, a large mosaic-VPH (290 mm x 475 mmelliptically-shaped recorded area), an f/1.4 six-element refractivecamera featuring silicon and fused silica elements with diameters aslarge as 393 mm, three near-infrared detectors mounted in a 1 x 3 mosaicwith sub-pixel translation capability, and all of these componentshoused within a custom, LN2-cooled, stainless steel vacuum cryostat withdimensions 1.4-m x 2.3-m x 1.3-m.</style></abstract><notes><style face="normal" font="default" size="100%">ISBN: &lt;ISBN&gt;9780819491473&lt;/ISBN&gt;</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1117/12.927140</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Aird, James</style></author><author><style face="normal" font="default" size="100%">Coil, Alison L.</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott M.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Smith, M. Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kenneth C. Wong</style></author><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">PRIMUS: The Dependence of AGN Accretion on Host Stellar Mass and Color</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">galaxies: active;  galaxies: evolution;  X-rays: galaxies</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJ...746...90A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">746</style></volume><pages><style face="normal" font="default" size="100%">90</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present evidence that the incidence of active galactic nuclei (AGNs)and the distribution of their accretion rates do not depend on thestellar masses of their host galaxies, contrary to previous studies. Weuse hard (2-10 keV) X-ray data from three extragalactic fields (XMM-LSS,COSMOS, and ELAIS-S1) with redshifts from the Prism Multi-object Surveyto identify 242 AGNs with L &lt;SUB&gt;2-10 keV&lt;/SUB&gt; = 10&lt;SUP&gt;42-44&lt;/SUP&gt; ergs&lt;SUP&gt;-1&lt;/SUP&gt; within a parent sample of ~25,000 galaxies at 0.2 &lt; z&lt; 1.0 over ~3.4 deg&lt;SUP&gt;2&lt;/SUP&gt; and to i ~ 23. We find that althoughthe fraction of galaxies hosting an AGN at fixed X-ray luminosity risesstrongly with stellar mass, the distribution of X-ray luminosities isindependent of mass. Furthermore, we show that the probability that agalaxy will host an AGN can be defined by a universal Eddington ratiodistribution that is independent of the host galaxy stellar mass and hasa power-law shape with slope -0.65. These results demonstrate that AGNsare prevalent at all stellar masses in the range 9.5 and that the samephysical processes regulate AGN activity in all galaxies in this stellarmass range. While a higher AGN fraction may be observed in massivegalaxies, this is a selection effect related to the underlying Eddingtonratio distribution. We also find that the AGN fraction drops rapidlybetween z ~ 1 and the present day and is moderately enhanced (factor ~2)in galaxies with blue or green optical colors. Consequently, while AGNactivity and star formation appear to be globally correlated, we do notfind evidence that the presence of an AGN is related to the quenching ofstar formation or the color transformation of galaxies.</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1107.4368</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ross, N. P.</style></author><author><style face="normal" font="default" size="100%">Myers, A. D.</style></author><author><style face="normal" font="default" size="100%">Sheldon, E. S.</style></author><author><style face="normal" font="default" size="100%">Yeche, C.</style></author><author><style face="normal" font="default" size="100%">Strauss, M. A.</style></author><author><style face="normal" font="default" size="100%">Bovy, J.</style></author><author><style face="normal" font="default" size="100%">Kirkpatrick, J. A.</style></author><author><style face="normal" font="default" size="100%">Richards, G. T.</style></author><author><style face="normal" font="default" size="100%">Aubourg, E.</style></author><author><style face="normal" font="default" size="100%">Blanton, M. R.</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Carithers, W. C.</style></author><author><style face="normal" font="default" size="100%">Croft, R. A. C.</style></author><author><style face="normal" font="default" size="100%">da Silva, R.</style></author><author><style face="normal" font="default" size="100%">Dawson, K.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Hennawi, J. F.</style></author><author><style face="normal" font="default" size="100%">Ho, S.</style></author><author><style face="normal" font="default" size="100%">Hogg, D. W.</style></author><author><style face="normal" font="default" size="100%">Lee, K.-G.</style></author><author><style face="normal" font="default" size="100%">Lundgren, B.</style></author><author><style face="normal" font="default" size="100%">McMahon, R. G.</style></author><author><style face="normal" font="default" size="100%">Miralda-Escude, J.</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, N.</style></author><author><style face="normal" font="default" size="100%">Paris, I.</style></author><author><style face="normal" font="default" size="100%">Petitjean, P.</style></author><author><style face="normal" font="default" size="100%">Pieri, M. M.</style></author><author><style face="normal" font="default" size="100%">Rich, J.</style></author><author><style face="normal" font="default" size="100%">Roe, N. A.</style></author><author><style face="normal" font="default" size="100%">Schiminovich, D.</style></author><author><style face="normal" font="default" size="100%">Schlegel, D. J.</style></author><author><style face="normal" font="default" size="100%">Schneider, D. P.</style></author><author><style face="normal" font="default" size="100%">Slosar, A. Z.</style></author><author><style face="normal" font="default" size="100%">Suzuki, N.</style></author><author><style face="normal" font="default" size="100%">Tinker, J. L.</style></author><author><style face="normal" font="default" size="100%">Weinberg, D. H.</style></author><author><style face="normal" font="default" size="100%">Weyant, A.</style></author><author><style face="normal" font="default" size="100%">White, M.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. M.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The quasars MMT-BOSS pilot survey (Ross+, 2012)</style></title><secondary-title><style face="normal" font="default" size="100%">VizieR Online Data Catalog</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Photometry: SDSS;  Redshifts;  QSOs;  Surveys</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012yCat..21990003R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">219</style></volume><pages><style face="normal" font="default" size="100%">90003</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey is now in its third phase (SDSS-III;Eisenstein et al. 2011AJ....142...72E) and is carrying out a combinationof four interleaved surveys that will continue until the summer of 2014.One of those surveys, the Baryon Oscillation Spectroscopic Survey(BOSS), commenced operations in late 2009 and is using essentially allthe dark time for SDSS-III. BOSS uses the same 2.5m Sloan Foundationtelescope that was used in SDSS-I/II, but since BOSS will observefainter targets, the fiber-fed spectrographs have been significantlyupgraded. These upgrades include: new CCDs with improved blue and redresponse; 1000 2&quot; instead of 640 3&quot; optical diameter fibers; higherthroughput gratings over a spectral range of 3600-10000Å at aresolution of about 2000, and improved optics.Prior to the commencement of BOSS spectroscopy, we carried outspectroscopy of quasar candidates selected from co-added photometry inSDSS Stripe 82. Observations of these candidates were carried out inqueue mode between 2008 September and 2009 January using the Hectospecmulti-fiber spectrograph on the 6.5m Multiple Mirror Telescope (MMT). InTables 14 and 15, we provide positions, PSF photometry (as observed,uncorrected for Galactic extinction), and redshifts for confirmedquasars from the MMT survey. Objects that are not flagged Primary in theCAS are listed separately (table 15).(2 data files).</style></abstract><notes><style face="normal" font="default" size="100%">table14.dat 437x94 Quasars discovered in the MMT survey; table15.dat 7x94 Quasars discovered in the MMT survey that are; non-primary in SDSS DR8 imaging</style></notes></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>47</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Beichman, Charles A.</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Greene, Thomas P.</style></author><author><style face="normal" font="default" size="100%">Krist, John</style></author><author><style face="normal" font="default" size="100%">McCarthy, Don</style></author><author><style face="normal" font="default" size="100%">Meyer, Michael</style></author><author><style face="normal" font="default" size="100%">Stansberry, John</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Science opportunities with the near-IR camera (NIRCam) on the James Webb Space Telescope (JWST)</style></title><secondary-title><style face="normal" font="default" size="100%">Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012SPIE.8442E..2NB</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">8442</style></volume><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The Near-Infrared Camera (NIRCam) on the James Webb Space Telescope(JWST) offers revolutionary gains in sensitivity throughout the 1-5μm region. NIRCam will enable great advances in all areas ofastrophysics, from the composition of objects in our own Kuiper Belt andthe physical properties of planets orbiting nearby stars to theformation of stars and the detection of the youngest galaxies in theUniverse. NIRCam also plays an important role in initial alignment ofJWST and the long term maintenance of its image quality. NIRCam ispresently undergoing instrument Integration and Test in preparation fordelivery to the JWST project. Key near-term milestones include thecompletion of cryogenic testing of the entire instrument; demonstrationof scientific and wavefront sensing performance requirements; testing ofreplacement H2RG detectors arrays; and an analysis of coronagraphicperformance in light of measured telescope wavefront characteristics.This paper summarizes the performance of NIRCam, the scientific andeducation/outreach goals of the science team, and some results of theon-going testing program.</style></abstract><notes><style face="normal" font="default" size="100%">ISBN: &lt;ISBN&gt;9780819491435&lt;/ISBN&gt;</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1117/12.925447</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Paris, I.</style></author><author><style face="normal" font="default" size="100%">Petitjean, P.</style></author><author><style face="normal" font="default" size="100%">Aubourg, E.</style></author><author><style face="normal" font="default" size="100%">Bailey, S.</style></author><author><style face="normal" font="default" size="100%">Ross, N. P.</style></author><author><style face="normal" font="default" size="100%">Myers, A. D.</style></author><author><style face="normal" font="default" size="100%">Strauss, M. A.</style></author><author><style face="normal" font="default" size="100%">Anderson, S. F.</style></author><author><style face="normal" font="default" size="100%">Arnau, E.</style></author><author><style face="normal" font="default" size="100%">Bautista, J.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, D.</style></author><author><style face="normal" font="default" size="100%">Bolton, A. S.</style></author><author><style face="normal" font="default" size="100%">Bovy, J.</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Brewington, H.</style></author><author><style face="normal" font="default" size="100%">Brownstein, J. R.</style></author><author><style face="normal" font="default" size="100%">Busca, N.</style></author><author><style face="normal" font="default" size="100%">Capellupo, D.</style></author><author><style face="normal" font="default" size="100%">Carithers, W.</style></author><author><style face="normal" font="default" size="100%">Croft, R. A. C.</style></author><author><style face="normal" font="default" size="100%">Dawson, K.</style></author><author><style face="normal" font="default" size="100%">Delubac, T.</style></author><author><style face="normal" font="default" size="100%">Ebelke, G.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Engelke, P.</style></author><author><style face="normal" font="default" size="100%">Fan, X.</style></author><author><style face="normal" font="default" size="100%">Filiz, Ak N.</style></author><author><style face="normal" font="default" size="100%">Finley, H.</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, A.</style></author><author><style face="normal" font="default" size="100%">Ge, J.</style></author><author><style face="normal" font="default" size="100%">Gibson, R. R.</style></author><author><style face="normal" font="default" size="100%">Hall, P. B.</style></author><author><style face="normal" font="default" size="100%">Hamann, F.</style></author><author><style face="normal" font="default" size="100%">Hennawi, J. F.</style></author><author><style face="normal" font="default" size="100%">Ho, S.</style></author><author><style face="normal" font="default" size="100%">Hogg, D. W.</style></author><author><style face="normal" font="default" size="100%">Ivezic, Z.</style></author><author><style face="normal" font="default" size="100%">Jiang, L.</style></author><author><style face="normal" font="default" size="100%">Kimball, A. E.</style></author><author><style face="normal" font="default" size="100%">Kirky, D.</style></author><author><style face="normal" font="default" size="100%">Kirkpatrick, J. A.</style></author><author><style face="normal" font="default" size="100%">Lee, K.-G.</style></author><author><style face="normal" font="default" size="100%">Le Goff, J.-M.</style></author><author><style face="normal" font="default" size="100%">Lundgren, B.</style></author><author><style face="normal" font="default" size="100%">MacLeod, C. L.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, E.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, V.</style></author><author><style face="normal" font="default" size="100%">Maraston, C.</style></author><author><style face="normal" font="default" size="100%">McGreer, I. D.</style></author><author><style face="normal" font="default" size="100%">McMahon, R. G.</style></author><author><style face="normal" font="default" size="100%">Miralda-Escude, J.</style></author><author><style face="normal" font="default" size="100%">Muna, D.</style></author><author><style face="normal" font="default" size="100%">Noterdaeme, P.</style></author><author><style face="normal" font="default" size="100%">Oravetz, D.</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, N.</style></author><author><style face="normal" font="default" size="100%">Pan, K.</style></author><author><style face="normal" font="default" size="100%">Perez-Fournon, I.</style></author><author><style face="normal" font="default" size="100%">Pieri, M. M.</style></author><author><style face="normal" font="default" size="100%">Richards, G. T.</style></author><author><style face="normal" font="default" size="100%">Rollinde, E.</style></author><author><style face="normal" font="default" size="100%">Sheldon, E. S.</style></author><author><style face="normal" font="default" size="100%">Schlegel, D. J.</style></author><author><style face="normal" font="default" size="100%">Schneider, D. P.</style></author><author><style face="normal" font="default" size="100%">Slosar, A.</style></author><author><style face="normal" font="default" size="100%">Shelden, A.</style></author><author><style face="normal" font="default" size="100%">Shen, Y.</style></author><author><style face="normal" font="default" size="100%">Simmons, A.</style></author><author><style face="normal" font="default" size="100%">Snedden, S.</style></author><author><style face="normal" font="default" size="100%">Suzuki, N.</style></author><author><style face="normal" font="default" size="100%">Tinker, J.</style></author><author><style face="normal" font="default" size="100%">Viel, M.</style></author><author><style face="normal" font="default" size="100%">Weaver, B. A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, D. W.</style></author><author><style face="normal" font="default" size="100%">White, M.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. M.</style></author><author><style face="normal" font="default" size="100%">Yeche, C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS Quasar Catalog, DR9Q (Paris+, 2012)</style></title><secondary-title><style face="normal" font="default" size="100%">VizieR Online Data Catalog</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Surveys;  QSOs;  Active gal. nuclei</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012yCat..35489066P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">354</style></volume><pages><style face="normal" font="default" size="100%">89066</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The SDSS-DR9 Quasar Catalog presents photometric and spectroscopicproperties of 87,822 quasars observed by the SDSS-III/BOSS survey. Weprovide the catalog in the form of a fits file but also an ascii file.We also provide a supplemental list containing 949 quasars with exactlythe same format as the main catalog.(4 data files).</style></abstract><notes><style face="normal" font="default" size="100%">dr9q.dat 87822x1174 Main DR9 Quasar catalog; dr9q.fits 29662x2880 Main DR9 Quasar catalog, FITS format; dr9qsup.dat 949x656 Supplemental list; dr9q_sup.fits 349x2880 Supplemental list, FITS format</style></notes></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin S.</style></author><author><style face="normal" font="default" size="100%">Yèche, Christophe</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Kirkpatrick, Jessica A.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Carithers, William C.</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">da Silva, Robert</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Lee, Khee-Gan</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">McMahon, Richard G.</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, Jordi</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Roe, Natalie A.</style></author><author><style face="normal" font="default" size="100%">Schiminovich, David</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Slosar, Anže</style></author><author><style face="normal" font="default" size="100%">Suzuki, Nao</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Weyant, Anya</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. Michael</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The SDSS-III Baryon Oscillation Spectroscopic Survey: Quasar Target Selection for Data Release Nine</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">cosmology: observations;  intergalactic medium;  quasars: absorption lines;  quasars: general;  surveys;  techniques: miscellaneous</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012ApJS..199....3R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">199</style></volume><pages><style face="normal" font="default" size="100%">3</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">The SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS), a five-yearspectroscopic survey of 10,000 deg&lt;SUP&gt;2&lt;/SUP&gt;, achieved first light inlate 2009. One of the key goals of BOSS is to measure the signature ofbaryon acoustic oscillations (BAOs) in the distribution of Lyαabsorption from the spectra of a sample of ~150,000 z &gt; 2.2 quasars.Along with measuring the angular diameter distance at z ≈ 2.5, BOSSwill provide the first direct measurement of the expansion rate of theuniverse at z &gt; 2. One of the biggest challenges in achieving thisgoal is an efficient target selection algorithm for quasars in theredshift range 2.2 &lt; z &lt; 3.5, where their colors tend to overlapthose of the far more numerous stars. During the first year of the BOSSsurvey, quasar target selection (QTS) methods were developed and testedto meet the requirement of delivering at least 15 quasarsdeg&lt;SUP&gt;-2&lt;/SUP&gt; in this redshift range, with a goal of 20 out of 40targets deg&lt;SUP&gt;-2&lt;/SUP&gt; allocated to the quasar survey. To achievethese surface densities, the magnitude limit of the quasar targets wasset at g &lt;= 22.0 or r &lt;= 21.85. While detection of the BAOsignature in the distribution of Lyα absorption in quasar spectradoes not require a uniform target selection algorithm, many otherastrophysical studies do. We have therefore defined a uniformly selectedsubsample of 20 targets deg&lt;SUP&gt;-2&lt;/SUP&gt;, for which the selection</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1105.0606</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Pâris, I.</style></author><author><style face="normal" font="default" size="100%">Petitjean, P.</style></author><author><style face="normal" font="default" size="100%">Aubourg, É.</style></author><author><style face="normal" font="default" size="100%">Bailey, S.</style></author><author><style face="normal" font="default" size="100%">Ross, N. P.</style></author><author><style face="normal" font="default" size="100%">Myers, A. D.</style></author><author><style face="normal" font="default" size="100%">Strauss, M. A.</style></author><author><style face="normal" font="default" size="100%">Anderson, S. F.</style></author><author><style face="normal" font="default" size="100%">Arnau, E.</style></author><author><style face="normal" font="default" size="100%">Bautista, J.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, D.</style></author><author><style face="normal" font="default" size="100%">Bolton, A. S.</style></author><author><style face="normal" font="default" size="100%">Bovy, J.</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Brewington, H.</style></author><author><style face="normal" font="default" size="100%">Browstein, J. R.</style></author><author><style face="normal" font="default" size="100%">Busca, N.</style></author><author><style face="normal" font="default" size="100%">Capellupo, D.</style></author><author><style face="normal" font="default" size="100%">Carithers, W.</style></author><author><style face="normal" font="default" size="100%">Croft, R. A. C.</style></author><author><style face="normal" font="default" size="100%">Dawson, K.</style></author><author><style face="normal" font="default" size="100%">Delubac, T.</style></author><author><style face="normal" font="default" size="100%">Ebelke, G.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Engelke, P.</style></author><author><style face="normal" font="default" size="100%">Fan, X.</style></author><author><style face="normal" font="default" size="100%">Filiz Ak, N.</style></author><author><style face="normal" font="default" size="100%">Finley, H.</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, A.</style></author><author><style face="normal" font="default" size="100%">Ge, J.</style></author><author><style face="normal" font="default" size="100%">Gibson, R. R.</style></author><author><style face="normal" font="default" size="100%">Hall, P. B.</style></author><author><style face="normal" font="default" size="100%">Hamann, F.</style></author><author><style face="normal" font="default" size="100%">Hennawi, J. F.</style></author><author><style face="normal" font="default" size="100%">Ho, S.</style></author><author><style face="normal" font="default" size="100%">Hogg, D. W.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Ž.</style></author><author><style face="normal" font="default" size="100%">Jiang, L.</style></author><author><style face="normal" font="default" size="100%">Kimball, A. E.</style></author><author><style face="normal" font="default" size="100%">Kirkby, D.</style></author><author><style face="normal" font="default" size="100%">Kirkpatrick, J. A.</style></author><author><style face="normal" font="default" size="100%">Lee, K.-G.</style></author><author><style face="normal" font="default" size="100%">Le Goff, J.-M.</style></author><author><style face="normal" font="default" size="100%">Lundgren, B.</style></author><author><style face="normal" font="default" size="100%">MacLeod, C. L.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, E.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, V.</style></author><author><style face="normal" font="default" size="100%">Maraston, C.</style></author><author><style face="normal" font="default" size="100%">McGreer, I. D.</style></author><author><style face="normal" font="default" size="100%">McMahon, R. G.</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, J.</style></author><author><style face="normal" font="default" size="100%">Muna, D.</style></author><author><style face="normal" font="default" size="100%">Noterdaeme, P.</style></author><author><style face="normal" font="default" size="100%">Oravetz, D.</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, N.</style></author><author><style face="normal" font="default" size="100%">Pan, K.</style></author><author><style face="normal" font="default" size="100%">Perez-Fournon, I.</style></author><author><style face="normal" font="default" size="100%">Pieri, M. M.</style></author><author><style face="normal" font="default" size="100%">Richards, G. T.</style></author><author><style face="normal" font="default" size="100%">Rollinde, E.</style></author><author><style face="normal" font="default" size="100%">Sheldon, E. S.</style></author><author><style face="normal" font="default" size="100%">Schlegel, D. J.</style></author><author><style face="normal" font="default" size="100%">Schneider, D. P.</style></author><author><style face="normal" font="default" size="100%">Slosar, A.</style></author><author><style face="normal" font="default" size="100%">Shelden, A.</style></author><author><style face="normal" font="default" size="100%">Shen, Y.</style></author><author><style face="normal" font="default" size="100%">Simmons, A.</style></author><author><style face="normal" font="default" size="100%">Snedden, S.</style></author><author><style face="normal" font="default" size="100%">Suzuki, N.</style></author><author><style face="normal" font="default" size="100%">Tinker, J.</style></author><author><style face="normal" font="default" size="100%">Viel, M.</style></author><author><style face="normal" font="default" size="100%">Weaver, B. A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, D. H.</style></author><author><style face="normal" font="default" size="100%">White, M.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. M.</style></author><author><style face="normal" font="default" size="100%">Yèche, C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey quasar catalog: ninth data release</style></title><secondary-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">catalogs;  surveys;  quasars: general</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012A%26A...548A..66P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">548</style></volume><pages><style face="normal" font="default" size="100%">66</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present the Data Release 9 Quasar (DR9Q) catalog from the BaryonOscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky SurveyIII. The catalog includes all BOSS objects that were targeted as quasarcandidates during the survey, are spectrocopically confirmed as quasarsvia visual inspection, have luminosities M&lt;SUB&gt;i&lt;/SUB&gt;[z = 2] &lt; -20.5(in a ΛCDM cosmology with H&lt;SUB&gt;0&lt;/SUB&gt; = 70 km s&lt;SUP&gt;-1&lt;/SUP&gt;Mpc&lt;SUP&gt;-1&lt;/SUP&gt;, Ω&lt;SUB&gt;M&lt;/SUB&gt; = 0.3, andΩ&lt;SUB&gt;Λ&lt;/SUB&gt; = 0.7) and either display at least oneemission line with full width at half maximum (FWHM) larger than 500 kms&lt;SUP&gt;-1&lt;/SUP&gt; or, if not, have interesting/complex absorption features.It includes as well, known quasars (mostly from SDSS-I and II) that werereobserved by BOSS. This catalog contains 87 822 quasars (78 086 are newdiscoveries) detected over 3275 deg&lt;SUP&gt;2&lt;/SUP&gt; with robustidentification and redshift measured by a combination of principalcomponent eigenspectra newly derived from a training set of 8632 spectrafrom SDSS-DR7. The number of quasars with z &gt; 2.15 (61 931) is ~2.8times larger than the number of z &gt; 2.15 quasars previously known.Redshifts and FWHMs are provided for the strongest emission lines (C iv,C iii], Mg ii). The catalog identifies 7533 broad absorption linequasars and gives their characteristics. For each object the catalogpresents five-band (u, g, r, i, z) CCD-based photometry with typicalaccuracy of 0.03 mag, and information on the morphology and selectionmethod. The catalog also contains X-ray, ultraviolet, near-infrared, andradio emission properties of the quasars, when available, from otherlarge-area surveys. The calibrated digital spectra cover the wavelengthregion 3600-10 500 Å at a spectral resolution in the range 1300&lt; R &lt; 2500; the spectra can be retrieved from the SDSS CatalogArchive Server. We also provide a supplemental list of an additional 949quasars that have been identified, among galaxy targets of the BOSS oramong quasar targets after DR9 was frozen.Catalog is only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via &lt;Ahref=&quot;http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/548/A66&quot;&gt;http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/548/A66&lt;/A&gt;</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1210.5166</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Bhardwaj, Vaishali</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Chen, Yan-Mei</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Olmstead, Matthew D.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shu, Yiping</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. Michael</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Spectral Classification and Redshift Measurement for the SDSS-III Baryon Oscillation Spectroscopic Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">methods: data analysis;  surveys;  techniques: spectroscopic</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2012</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2012</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2012AJ....144..144B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">144</style></volume><pages><style face="normal" font="default" size="100%">144</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We describe the automated spectral classification, redshiftdetermination, and parameter measurement pipeline in use for the BaryonOscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky SurveyIII (SDSS-III) as of the survey's ninth data release (DR9), encompassing831,000 moderate-resolution optical spectra. We give a review of thealgorithms employed, and describe the changes to the pipeline that havebeen implemented for BOSS relative to previous SDSS-I/II versions,including new sets of stellar, galaxy, and quasar redshift templates.For the color-selected &quot;CMASS&quot; sample of massive galaxies at redshift0.4 &lt;~ z &lt;~ 0.8 targeted by BOSS for the purposes of large-scalecosmological measurements, the pipeline achieves an automated</style></abstract><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1207.7326</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hickox, Ryan C.</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Brodwin, Mark</style></author><author><style face="normal" font="default" size="100%">Alexander, David M.</style></author><author><style face="normal" font="default" size="100%">Forman, William R.</style></author><author><style face="normal" font="default" size="100%">Jones, Christine</style></author><author><style face="normal" font="default" size="100%">Murray, Stephen S.</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Assef, Roberto J.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, Peter R.</style></author><author><style face="normal" font="default" size="100%">Gorjian, Varoujan</style></author><author><style face="normal" font="default" size="100%">Stern, Daniel</style></author><author><style face="normal" font="default" size="100%">Le Floc'h, Emeric</style></author><author><style face="normal" font="default" size="100%">Caldwell, Nelson</style></author><author><style face="normal" font="default" size="100%">Goulding, Andrew D.</style></author><author><style face="normal" font="default" size="100%">Mullaney, James R.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Clustering of Obscured and Unobscured Quasars in the Boötes Field: Placing Rapidly Growing Black Holes in the Cosmic Web</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...731..117H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">731</style></volume><pages><style face="normal" font="default" size="100%">117</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the first measurement of the spatial clustering ofmid-infrared-selected obscured and unobscured quasars, using a sample inthe redshift range 0.7 &amp;lt; z &amp;lt; 1.8 selected from the 9deg&lt;sup&gt;2&lt;/sup&gt; Boötes multiwavelength survey. Recently, theSpitzer Space Telescope and X-ray observations have revealed largepopulations of obscured quasars that have been inferred from models ofthe X-ray background and supermassive black hole evolution. To date,little is known about obscured quasar clustering, which allows us tomeasure the masses of their host dark matter halos and explore theirrole in the cosmic evolution of black holes and galaxies. In this study,we use a sample of 806 mid-infrared-selected quasars and ≈250,000galaxies to calculate the projected quasar-galaxy cross-correlationfunction w&lt;sub&gt;p&lt;/sub&gt; (R). The observed clustering yieldscharacteristic dark matter halo masses of log(M &lt;sub&gt;halo&lt;/sub&gt; [h&lt;sup&gt;-1&lt;/sup&gt; M &lt;sub&gt;sun&lt;/sub&gt;]) = 12.7&lt;sup&gt;+0.4&lt;/sup&gt; &lt;sub&gt;-0.6&lt;/sub&gt;and 13.3&lt;sup&gt;+0.3&lt;/sup&gt; &lt;sub&gt;-0.4&lt;/sub&gt; for unobscured quasars (QSO-1s)and obscured quasars (Obs-QSOs), respectively. The results for QSO-1sare in excellent agreement with previous measurements for opticallyselected quasars, while we conclude that the Obs-QSOs are at least asstrongly clustered as the QSO-1s. We test for the effects of photometricredshift errors on the optically faint Obs-QSOs, and find that ourmethod yields a robust lower limit on the clustering; photo-z errors maycause us to underestimate the clustering amplitude of the Obs-QSOs by at&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1102.4850</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Starikova, S.</style></author><author><style face="normal" font="default" size="100%">Cool, R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Forman, W.</style></author><author><style face="normal" font="default" size="100%">Jones, C.</style></author><author><style face="normal" font="default" size="100%">Hickox, R.</style></author><author><style face="normal" font="default" size="100%">Kenter, A.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C.</style></author><author><style face="normal" font="default" size="100%">Kravtsov, A.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Vikhlinin, A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Constraining Halo Occupation Properties of X-Ray Active Galactic Nuclei Using Clustering of Chandra Sources in the Boötes Survey Region</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...741...15S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">741</style></volume><pages><style face="normal" font="default" size="100%">15</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present one of the most precise measurements to date of the spatialclustering of X-ray-selected active galactic nuclei (AGNs) using asample derived from the Chandra X-ray Observatory survey in theBoötes field. The real-space two-point correlation function over aredshift interval from z = 0.17 to z ~ 3 is well described by the powerlaw, ξ(r) = (r/r &lt;sub&gt;0&lt;/sub&gt;)&lt;sup&gt;-γ&lt;/sup&gt;, for comovingseparations r &amp;lt;~ 20 h &lt;sup&gt;-1&lt;/sup&gt; Mpc. We find γ = 1.84± 0.12 and r &lt;sub&gt;0&lt;/sub&gt; consistent with no redshift trendwithin the sample (varying between r &lt;sub&gt;0&lt;/sub&gt; = 5.5 ± 0.6 h&lt;sup&gt;-1&lt;/sup&gt; Mpc for langzrang = 0.37 and r &lt;sub&gt;0&lt;/sub&gt; = 6.9± 1.0 h &lt;sup&gt;-1&lt;/sup&gt; Mpc for langzrang = 1.28).Furthermore, we are able to measure the projections of the two-pointcorrelation function both on the sky plane and in the line of sight. Weuse these measurements to show that the Chandra/Boötes AGNs arepredominantly located at the centers of dark matter halos with circularvelocity v &lt;sub&gt;max&lt;/sub&gt; &amp;gt; 320 km s&lt;sup&gt;-1&lt;/sup&gt; or M&lt;sub&gt;180&lt;/sub&gt; &amp;gt; 4.1 × 10&lt;sup&gt;12&lt;/sup&gt; h &lt;sup&gt;-1&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, and tend to avoid satellite galaxies in halos of this orhigher mass. The halo occupation properties inferred from the clusteringproperties of Chandra/Boötes AGNs—the mass scale of theparent dark matter halos, the lack of significant redshift evolution ofthe clustering length, and the low satellite fraction—are broadlyconsistent with the Hopkins et al. scenario of quasar activity triggeredby mergers of similarly sized galaxies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1010.1577</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Aihara, Hiroaki</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">An, Deokkeun</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Balbinot, Eduardo</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bickerton, Steven J.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brown, Peter J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Busca, Nicolas G.</style></author><author><style face="normal" font="default" size="100%">Campbell, Heather</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Chen, Yanmei</style></author><author><style face="normal" font="default" size="100%">Chiappini, Cristina</style></author><author><style face="normal" font="default" size="100%">Comparat, Johan</style></author><author><style face="normal" font="default" size="100%">Connolly, Natalia</style></author><author><style face="normal" font="default" size="100%">Cortes, Marina</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">Cuesta, Antonio J.</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz N.</style></author><author><style face="normal" font="default" size="100%">Davenport, James R. A.</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle</style></author><author><style face="normal" font="default" size="100%">Dhital, Saurav</style></author><author><style face="normal" font="default" size="100%">Ealet, Anne</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett L.</style></author><author><style face="normal" font="default" size="100%">Edmondson, Edward M.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Escoffier, Stephanie</style></author><author><style face="normal" font="default" size="100%">Esposito, Massimiliano</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Femenía Castellá, Bruno</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, Peter M.</style></author><author><style face="normal" font="default" size="100%">Ge, Jian</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce A.</style></author><author><style face="normal" font="default" size="100%">Gilmore, G.</style></author><author><style face="normal" font="default" size="100%">González Hernández, Jonay I.</style></author><author><style face="normal" font="default" size="100%">Gott, J. Richard</style></author><author><style face="normal" font="default" size="100%">Gould, Andrew</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Harding, Paul</style></author><author><style face="normal" font="default" size="100%">Harris, David W.</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hearty, Frederick R.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Ivans, Inese I.</style></author><author><style face="normal" font="default" size="100%">Jiang, Linhua</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Jordan, Cathy</style></author><author><style face="normal" font="default" size="100%">Jordan, Wendell P.</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal A.</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Klaene, Mark A.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kneib, Jean-Paul</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Koesterke, Lars</style></author><author><style face="normal" font="default" size="100%">Kollmeier, Juna A.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lang, Dustin</style></author><author><style face="normal" font="default" size="100%">Le Goff, Jean-Marc</style></author><author><style face="normal" font="default" size="100%">Lee, Young Sun</style></author><author><style face="normal" font="default" size="100%">Lin, Yen-Ting</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Lucatello, Sara</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Ma, Zhibo</style></author><author><style face="normal" font="default" size="100%">MacDonald, Nicholas</style></author><author><style face="normal" font="default" size="100%">Mahadevan, Suvrath</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio A. G.</style></author><author><style face="normal" font="default" size="100%">Makler, Martin</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Margala, Daniel</style></author><author><style face="normal" font="default" size="100%">Masters, Karen L.</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McGreer, Ian D.</style></author><author><style face="normal" font="default" size="100%">Ménard, Brice</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, Jordi</style></author><author><style face="normal" font="default" size="100%">Morrison, Heather L.</style></author><author><style face="normal" font="default" size="100%">Mullally, F.</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Murayama, Hitoshi</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Naugle, Tracy</style></author><author><style face="normal" font="default" size="100%">Fausti Neto, Angelo</style></author><author><style face="normal" font="default" size="100%">Cuong Nguyen, Duy</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Robert W.</style></author><author><style face="normal" font="default" size="100%">Ogando, Ricardo L. C.</style></author><author><style face="normal" font="default" size="100%">Olmstead, Matthew D.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Pandey, Parul</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Pfaffenberger, Robert</style></author><author><style face="normal" font="default" size="100%">Pforr, Janine</style></author><author><style face="normal" font="default" size="100%">Phleps, Stefanie</style></author><author><style face="normal" font="default" size="100%">Pichon, Christophe</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Price-Whelan, Adrian M.</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Ramos, Beatriz H. F.</style></author><author><style face="normal" font="default" size="100%">Reylé, Céline</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Robin, Annie C.</style></author><author><style face="normal" font="default" size="100%">Rocha-Pinto, Helio J.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Roe, Natalie A.</style></author><author><style face="normal" font="default" size="100%">Rollinde, Emmanuel</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Rossetto, Bruno M.</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Sayres, Conor</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schlesinger, Katharine J.</style></author><author><style face="normal" font="default" size="100%">Schmidt, Sarah J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shu, Yiping</style></author><author><style face="normal" font="default" size="100%">Simmerer, Jennifer</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey E.</style></author><author><style face="normal" font="default" size="100%">Sivarani, Thirupathi</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Sobeck, Jennifer S.</style></author><author><style face="normal" font="default" size="100%">Steinmetz, Matthias</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Tanaka, Masayuki</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tofflemire, Benjamin M.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, M.</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Wang, Ji</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yasuda, Naoki</style></author><author><style face="normal" font="default" size="100%">Yeche, Christophe</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Eighth Data Release of the Sloan Digital Sky Survey: First Data from SDSS-III</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJS..193...29A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">193</style></volume><pages><style face="normal" font="default" size="100%">29</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Sloan Digital Sky Survey (SDSS) started a new phase in 2008 August,with new instrumentation and new surveys focused on Galactic structureand chemical evolution, measurements of the baryon oscillation featurein the clustering of galaxies and the quasar Lyα forest, and aradial velocity search for planets around ~8000 stars. This paperdescribes the first data release of SDSS-III (and the eighth countingfrom the beginning of the SDSS). The release includes five-band imagingof roughly 5200 deg&lt;sup&gt;2&lt;/sup&gt; in the southern Galactic cap, bringingthe total footprint of the SDSS imaging to 14,555 deg&lt;sup&gt;2&lt;/sup&gt;, orover a third of the Celestial Sphere. All the imaging data have beenreprocessed with an improved sky-subtraction algorithm and a final,self-consistent photometric recalibration and flat-field determination.This release also includes all data from the second phase of the SloanExtension for Galactic Understanding and Exploration (SEGUE-2),consisting of spectroscopy of approximately 118,000 stars at both highand low Galactic latitudes. All the more than half a million stellarspectra obtained with the SDSS spectrograph have been reprocessedthrough an improved stellar parameter pipeline, which has betterdetermination of metallicity for high-metallicity stars.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1101.1559</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Mehta, Kushal T.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eckel, Jonathan</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Metchnik, Marc</style></author><author><style face="normal" font="default" size="100%">Pinto, Philip</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Galaxy Bias and Its Effects on the Baryon Acoustic Oscillation Measurements</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...734...94M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">734</style></volume><pages><style face="normal" font="default" size="100%">94</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The baryon acoustic oscillation (BAO) feature in the clustering ofmatter in the universe serves as a robust standard ruler and hence canbe used to map the expansion history of the universe. We use high forceresolution simulations to analyze the effects of galaxy bias on themeasurements of the BAO signal. We apply a variety of Halo OccupationDistributions (HODs) and produce biased mass tracers to mimic differentgalaxy populations. We investigate whether galaxy bias changes thenonlinear shifts on the acoustic scale relative to the underlying darkmatter distribution presented by Seo et al. For the less biased HODmodels (b &amp;lt; 3), we do not detect any shift in the acoustic scale&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1104.1178</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Yang, Yujin</style></author><author><style face="normal" font="default" size="100%">Zabludoff, Ann</style></author><author><style face="normal" font="default" size="100%">Jahnke, Knud</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Davé, Romeel</style></author><author><style face="normal" font="default" size="100%">Shectman, Stephen A.</style></author><author><style face="normal" font="default" size="100%">Kelson, Daniel D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Gas Kinematics in Lyα Nebulae</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...735...87Y</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">735</style></volume><pages><style face="normal" font="default" size="100%">87</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Exploring the origin of Lyα nebulae (&quot;blobs&quot;) at high redshiftrequires measurements of their gas kinematics that are impossible withonly the resonant, optically thick Lyα line. To define gas motionsrelative to the systemic velocity of the blob, the Lyα line mustbe compared with an optically thin line like Hα λ6563,which is not much altered by radiative transfer effects and is moreconcentrated about the galaxies embedded in the nebula's core. We obtainoptical and near-IR (NIR) spectra of the two brightest Lyα blobs(CDFS-LAB01 and CDFS-LAB02) from the Yang et al. sample using theMagellan/Magellan Echellette Spectrograph optical and Very LargeTelescope/SINFONI NIR spectrographs. Both the Lyα and Hαlines confirm that these blobs lie at the survey redshift, z ~ 2.3.Within each blob, we detect several Hα sources, which roughlycorrespond to galaxies seen in Hubble Space Telescope rest-frame UVimages. The Hα detections show that these galaxies have largeinternal velocity dispersions (σ&lt;sub&gt; v &lt;/sub&gt; = 130-190 kms&lt;sup&gt;-1&lt;/sup&gt;) and that, in the one system (LAB01), where we canreliably extract profiles for two Hα sources, their velocitydifference is Δv ~ 440 km s&lt;sup&gt;-1&lt;/sup&gt;. The presence of multiplegalaxies within the blobs, and those galaxies' large velocitydispersions and large relative motion, is consistent with our previousfinding that Lyα blobs inhabit massive dark matter halos that willevolve into those typical of present-day rich clusters and that theembedded galaxies may eventually become brightest cluster galaxies. Todetermine whether the gas near the embedded galaxies is predominantlyinfalling or outflowing, we compare the Lyα and Hα linecenters, finding that Lyα is not offset (Δv&lt;sub&gt;Lyα&lt;/sub&gt; = +0 km s&lt;sup&gt;-1&lt;/sup&gt;) in LAB01 and redshifted byonly +230 km s&lt;sup&gt;-1&lt;/sup&gt; in LAB02. These offsets are small comparedto those of Lyman break galaxies, which average +450 km s&lt;sup&gt;-1&lt;/sup&gt;and extend to about +700 km s&lt;sup&gt;-1&lt;/sup&gt;. In LAB02, we detect C IIλ1334 and Si II λ1526 absorption lines, whose bluewardshifts of ~200 km s&lt;sup&gt;-1&lt;/sup&gt; are consistent with the small outflowimplied by the redward shift of Lyα. We test and rule out thesimplest infall models and those outflow models with super/hyperwinds,which require large outflow velocities. Because of the unknown geometryof the gas distribution and the possibility of multiple sources ofLyα emission embedded in the blobs, a larger sample and moresophisticated models are required to test more complex or a wider rangeof infall and outflow scenarios.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1104.3597</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Slosar, Anže</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Le Goff, Jean-Marc</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Busca, Nicolas</style></author><author><style face="normal" font="default" size="100%">Carithers, Bill</style></author><author><style face="normal" font="default" size="100%">Charlassier, Romain</style></author><author><style face="normal" font="default" size="100%">Cortês, Marina</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle S.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Lee, Khee-Gan</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert</style></author><author><style face="normal" font="default" size="100%">McDonald, Patrick</style></author><author><style face="normal" font="default" size="100%">Medolin, Bumbarija</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, Jordi</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Piškur, Yodovina</style></author><author><style face="normal" font="default" size="100%">Rollinde, Emmanuel</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Yeche, Christophe</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Lyman-α forest in three dimensions: measurements of large scale flux correlations from BOSS 1st-year data</style></title><secondary-title><style face="normal" font="default" size="100%">Journal of Cosmology and Astro-Particle Physics</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011JCAP...09..001S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">09</style></volume><pages><style face="normal" font="default" size="100%">001</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Using a sample of approximately 14,000 z &amp;gt; 2.1 quasars observed inthe first year of the Baryon Oscillation Spectroscopic Survey (BOSS), wemeasure the three-dimensional correlation function of absorption in theLyman-α forest. The angle-averaged correlation function oftransmitted flux (F = e&lt;sup&gt;-τ&lt;/sup&gt;) is securely detected outto comoving separations of 60 h&lt;sup&gt;-1&lt;/sup&gt;Mpc, the firstdetection of flux correlations across widely separated sightlines. Aquadrupole distortion of the redshift-space correlation function bypeculiar velocities, the signature of the gravitational instabilityorigin of structure in the Lyman-α forest, is also detected athigh significance. We obtain a good fit to the data assuming lineartheory redshift-space distortion and linear bias of the transmittedflux, relative to the matter fluctuations of a standard ΛCDMcosmological model (inflationary cold dark matter with a cosmological&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1104.5244</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Lee, Brian L.</style></author><author><style face="normal" font="default" size="100%">Ge, Jian</style></author><author><style face="normal" font="default" size="100%">Fleming, Scott W.</style></author><author><style face="normal" font="default" size="100%">Stassun, Keivan G.</style></author><author><style face="normal" font="default" size="100%">Gaudi, B. Scott</style></author><author><style face="normal" font="default" size="100%">Barnes, Rory</style></author><author><style face="normal" font="default" size="100%">Mahadevan, Suvrath</style></author><author><style face="normal" font="default" size="100%">Eastman, Jason D.</style></author><author><style face="normal" font="default" size="100%">Wright, Jason</style></author><author><style face="normal" font="default" size="100%">Siverd, Robert J.</style></author><author><style face="normal" font="default" size="100%">Gary, Bruce</style></author><author><style face="normal" font="default" size="100%">Ghezzi, Luan</style></author><author><style face="normal" font="default" size="100%">Laws, Chris</style></author><author><style face="normal" font="default" size="100%">Wisniewski, John P.</style></author><author><style face="normal" font="default" size="100%">Porto de Mello, G. F.</style></author><author><style face="normal" font="default" size="100%">Ogando, Ricardo L. C.</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio A. G.</style></author><author><style face="normal" font="default" size="100%">Nicolaci da Costa, Luiz</style></author><author><style face="normal" font="default" size="100%">Sivarani, Thirupathi</style></author><author><style face="normal" font="default" size="100%">Pepper, Joshua</style></author><author><style face="normal" font="default" size="100%">Cuong Nguyen, Duy</style></author><author><style face="normal" font="default" size="100%">Hebb, Leslie</style></author><author><style face="normal" font="default" size="100%">De Lee, Nathan</style></author><author><style face="normal" font="default" size="100%">Wang, Ji</style></author><author><style face="normal" font="default" size="100%">Wan, Xiaoke</style></author><author><style face="normal" font="default" size="100%">Zhao, Bo</style></author><author><style face="normal" font="default" size="100%">Chang, Liang</style></author><author><style face="normal" font="default" size="100%">Groot, John</style></author><author><style face="normal" font="default" size="100%">Varosi, Frank</style></author><author><style face="normal" font="default" size="100%">Hearty, Fred</style></author><author><style face="normal" font="default" size="100%">Hanna, Kevin</style></author><author><style face="normal" font="default" size="100%">van Eyken, J. C.</style></author><author><style face="normal" font="default" size="100%">Kane, Stephen R.</style></author><author><style face="normal" font="default" size="100%">Agol, Eric</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Chen, Zhiping</style></author><author><style face="normal" font="default" size="100%">Costello, Erin</style></author><author><style face="normal" font="default" size="100%">Dou, Liming</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Fletcher, Adam</style></author><author><style face="normal" font="default" size="100%">Ford, Eric B.</style></author><author><style face="normal" font="default" size="100%">Guo, Pengcheng</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Jiang, Peng</style></author><author><style face="normal" font="default" size="100%">French Leger, R.</style></author><author><style face="normal" font="default" size="100%">Liu, Jian</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Malik, Mohit</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Rohan, Pais</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey</style></author><author><style face="normal" font="default" size="100%">Weaver, B. A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Xie, Ji-Wei</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">MARVELS-1b: A Short-period, Brown Dwarf Desert Candidate from the SDSS-III Marvels Planet Search</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...728...32L</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">728</style></volume><pages><style face="normal" font="default" size="100%">32</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a new short-period brown dwarf (BD) candidate around the starTYC 1240-00945-1. This candidate was discovered in the first year of theMulti-object APO Radial Velocity Exoplanets Large-area Survey (MARVELS),which is part of the Sloan Digital Sky Survey (SDSS) III, and wedesignate the BD as MARVELS-1b. MARVELS uses the technique of dispersedfixed-delay interferometery to simultaneously obtain radial velocity(RV) measurements for 60 objects per field using a single, custom-builtinstrument that is fiber fed from the SDSS 2.5 m telescope. From our 20RV measurements spread over a ~370 day time baseline, we derive aKeplerian orbital fit with semi-amplitude K = 2.533 ± 0.025 kms&lt;sup&gt;-1&lt;/sup&gt;, period P = 5.8953 ± 0.0004 days, and eccentricityconsistent with circular. Independent follow-up RV data confirm theorbit. Adopting a mass of 1.37 ± 0.11 M &lt;sub&gt;sun&lt;/sub&gt; for theslightly evolved F9 host star, we infer that the companion has a minimummass of 28.0 ± 1.5 M &lt;sub&gt;Jup&lt;/sub&gt;, a semimajor axis 0.071± 0.002 AU assuming an edge-on orbit, and is probably tidallysynchronized. We find no evidence for coherent intrinsic variability ofthe host star at the period of the companion at levels greater than afew millimagnitudes. The companion has an a priori transit probability&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1011.5170</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Rujopakarn, Wiphu</style></author><author><style face="normal" font="default" size="100%">Rieke, George H.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Juneau, Stéphanie</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Morphology and Size Differences Between Local and High-redshift Luminous Infrared Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...726...93R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">726</style></volume><pages><style face="normal" font="default" size="100%">93</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We show that the star-forming regions in high-redshift luminous andultraluminous infrared galaxies (LIRGs and ULIRGs) and submillimetergalaxies (SMGs) have similar physical scales to those in local normalstar-forming galaxies. To first order, their higher infrared (IR)luminosities result from higher luminosity surface density. We also finda good correlation between the IR luminosity and IR luminosity surfacedensity in starburst galaxies across over five orders of magnitude of IRluminosity from local normal galaxies to z ~ 2 SMGs. The intenselystar-forming regions of local ULIRGs are significantly smaller thanthose in their high-redshift counterparts and hence divergesignificantly from this correlation, indicating that the ULIRGs foundlocally are a different population from the high-redshift ULIRGs andSMGs. Based on this relationship, we suggest that luminosity surfacedensity should serve as a more accurate indicator for the IR emittingenvironment, and hence the observable properties, of star-forminggalaxies than their IR luminosity. We demonstrate this approach byshowing that ULIRGs at z ~ 1 and a lensed galaxy at z ~ 2.5 exhibitaromatic features agreeing with local LIRGs that are an order ofmagnitude less luminous, but have similar IR luminosity surface density.A consequence of this relationship is that the aromatic emissionstrength in star-forming galaxies will appear to increase at z&amp;gt;1 fora given IR luminosity compared to their local counterparts.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1010.0675</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kenneth C. Wong</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott M.</style></author><author><style face="normal" font="default" size="100%">Coil, Alison L.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author><author><style face="normal" font="default" size="100%">Arnouts, Stéphane</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">PRIMUS: Enhanced Specific Star Formation Rates in Close Galaxy Pairs</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...728..119W</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">728</style></volume><pages><style face="normal" font="default" size="100%">119</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Tidal interactions between galaxies can trigger star formation, whichcontributes to the global star formation rate (SFR) density of theuniverse and could be a factor in the transformation of blue,star-forming galaxies to red, quiescent galaxies over cosmic time. Weinvestigate tidally triggered star formation in isolated close galaxypairs drawn from the Prism Multi-Object Survey (PRIMUS), alow-dispersion prism redshift survey that has measured ~120,000 robustgalaxy redshifts over 9.1 deg&lt;sup&gt;2&lt;/sup&gt; out to z ~ 1. We select asample of galaxies in isolated galaxy pairs at redshifts 0.25 &amp;lt;= z&amp;lt;= 0.75, with no other objects within a projected separation of 300 h&lt;sup&gt;-1&lt;/sup&gt; kpc and Δz/(1 + z) = 0.01, and compare them to acontrol sample of isolated galaxies to test for systematic differencesin their rest-frame FUV - r and NUV - r colors as a proxy for relativespecific star formation rates (SSFRs). We find that galaxies inr&lt;sub&gt;p&lt;/sub&gt; &amp;lt;= 50 h &lt;sup&gt;-1&lt;/sup&gt; kpc pairs have bluerdust-corrected UV - r colors on average than the control galaxies by-0.134 ± 0.045 mag in FUV - r and -0.075 ± 0.038 mag in&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1012.1324</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott M.</style></author><author><style face="normal" font="default" size="100%">Coil, Alison L.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Kenneth C. Wong</style></author><author><style face="normal" font="default" size="100%">Aird, James</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">PRIMUS: Obscured Star Formation on the Red Sequence</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...726..110Z</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">726</style></volume><pages><style face="normal" font="default" size="100%">110</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We quantify the fraction of galaxies at moderate redshifts (0.1 &amp;lt; z&amp;lt; 0.5) that appear red-and-dead in the optical, but in fact containobscured star formation detectable in the infrared (IR), with the PRIsmMUlti-object Survey (PRIMUS). PRIMUS has measured ~120,000 robust&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1011.4308</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Coil, Alison L.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott M.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Kenneth C. Wong</style></author><author><style face="normal" font="default" size="100%">Zhu, Guangtun</style></author><author><style face="normal" font="default" size="100%">Aird, James</style></author><author><style face="normal" font="default" size="100%">Bernstein, Rebecca A.</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The PRIsm MUlti-object Survey (PRIMUS). I. Survey Overview and Characteristics</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2011</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011ApJ...741....8C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">741</style></volume><pages><style face="normal" font="default" size="100%">8</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the PRIsm MUlti-object Survey (PRIMUS), a spectroscopic faintgalaxy redshift survey to z ~ 1. PRIMUS uses a low-dispersion prism andslitmasks to observe ~2500 objects at once in a 0.18 deg&lt;sup&gt;2&lt;/sup&gt;field of view, using the Inamori Magellan Areal Camera and Spectrographcamera on the Magellan I Baade 6.5 m telescope at Las CampanasObservatory. PRIMUS covers a total of 9.1 deg&lt;sup&gt;2&lt;/sup&gt; of sky to adepth of i &lt;sub&gt;AB&lt;/sub&gt; ~ 23.5 in seven different deep,multi-wavelength fields that have coverage from the Galaxy EvolutionExplorer, Spitzer, and either XMM or Chandra, as well as multiple-bandoptical and near-IR coverage. PRIMUS includes ~130,000 robust redshiftsof unique objects with a redshift precision of σ&lt;sub&gt; z &lt;/sub&gt;/(1+ z) ~ 0.005. The redshift distribution peaks at z ~ 0.6 and extends toz = 1.2 for galaxies and z = 5 for broad-line active galactic nuclei.The motivation, observational techniques, fields, target selection,slitmask design, and observations are presented here, with a briefsummary of the redshift precision; a forthcoming paper presents the datareduction, redshift fitting, redshift confidence, and surveycompleteness. PRIMUS is the largest faint galaxy survey undertaken to&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1011.4307</style></custom3><reprint-edition><style face="normal" font="default" size="100%">structure to z ~ 1.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Agol, Eric</style></author><author><style face="normal" font="default" size="100%">Aihara, Hiroaki</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Arns, James A.</style></author><author><style face="normal" font="default" size="100%">Aubourg, Éric</style></author><author><style face="normal" font="default" size="100%">Bailey, Stephen</style></author><author><style face="normal" font="default" size="100%">Balbinot, Eduardo</style></author><author><style face="normal" font="default" size="100%">Barkhouser, Robert</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bickerton, Steven J.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Bosman, Casey T.</style></author><author><style face="normal" font="default" size="100%">Bovy, Jo</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Breslauer, Ben</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brown, Peter J.</style></author><author><style face="normal" font="default" size="100%">Brownstein, Joel R.</style></author><author><style face="normal" font="default" size="100%">Burger, Dan</style></author><author><style face="normal" font="default" size="100%">Busca, Nicolas G.</style></author><author><style face="normal" font="default" size="100%">Campbell, Heather</style></author><author><style face="normal" font="default" size="100%">Cargile, Phillip A.</style></author><author><style face="normal" font="default" size="100%">Carithers, William C.</style></author><author><style face="normal" font="default" size="100%">Carlberg, Joleen K.</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Chang, Liang</style></author><author><style face="normal" font="default" size="100%">Chen, Yanmei</style></author><author><style face="normal" font="default" size="100%">Chiappini, Cristina</style></author><author><style face="normal" font="default" size="100%">Comparat, Johan</style></author><author><style face="normal" font="default" size="100%">Connolly, Natalia</style></author><author><style face="normal" font="default" size="100%">Cortes, Marina</style></author><author><style face="normal" font="default" size="100%">Croft, Rupert A. C.</style></author><author><style face="normal" font="default" size="100%">Cunha, Katia</style></author><author><style face="normal" font="default" size="100%">da Costa, Luiz N.</style></author><author><style face="normal" font="default" size="100%">Davenport, James R. A.</style></author><author><style face="normal" font="default" size="100%">Dawson, Kyle</style></author><author><style face="normal" font="default" size="100%">De Lee, Nathan</style></author><author><style face="normal" font="default" size="100%">Porto de Mello, Gustavo F.</style></author><author><style face="normal" font="default" size="100%">de Simoni, Fernando</style></author><author><style face="normal" font="default" size="100%">Dean, Janice</style></author><author><style face="normal" font="default" size="100%">Dhital, Saurav</style></author><author><style face="normal" font="default" size="100%">Ealet, Anne</style></author><author><style face="normal" font="default" size="100%">Ebelke, Garrett L.</style></author><author><style face="normal" font="default" size="100%">Edmondson, Edward M.</style></author><author><style face="normal" font="default" size="100%">Eiting, Jacob M.</style></author><author><style face="normal" font="default" size="100%">Escoffier, Stephanie</style></author><author><style face="normal" font="default" size="100%">Esposito, Massimiliano</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Femenía Castellá, Bruno</style></author><author><style face="normal" font="default" size="100%">Dutra Ferreira, Leticia</style></author><author><style face="normal" font="default" size="100%">Fitzgerald, Greg</style></author><author><style face="normal" font="default" size="100%">Fleming, Scott W.</style></author><author><style face="normal" font="default" size="100%">Font-Ribera, Andreu</style></author><author><style face="normal" font="default" size="100%">Ford, Eric B.</style></author><author><style face="normal" font="default" size="100%">Frinchaboy, Peter M.</style></author><author><style face="normal" font="default" size="100%">Elia García Pérez, Ana</style></author><author><style face="normal" font="default" size="100%">Gaudi, B. Scott</style></author><author><style face="normal" font="default" size="100%">Ge, Jian</style></author><author><style face="normal" font="default" size="100%">Ghezzi, Luan</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce A.</style></author><author><style face="normal" font="default" size="100%">Gilmore, G.</style></author><author><style face="normal" font="default" size="100%">Girardi, Léo</style></author><author><style face="normal" font="default" size="100%">Gott, J. Richard</style></author><author><style face="normal" font="default" size="100%">Gould, Andrew</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hamilton, Jean-Christophe</style></author><author><style face="normal" font="default" size="100%">Harding, Paul</style></author><author><style face="normal" font="default" size="100%">Harris, David W.</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hearty, Frederick R.</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">González Hernández, Jonay I.</style></author><author><style face="normal" font="default" size="100%">Ho, Shirley</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Honscheid, Klaus</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Ivans, Inese I.</style></author><author><style face="normal" font="default" size="100%">Jiang, Linhua</style></author><author><style face="normal" font="default" size="100%">Jiang, Peng</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Jordan, Cathy</style></author><author><style face="normal" font="default" size="100%">Jordan, Wendell P.</style></author><author><style face="normal" font="default" size="100%">Kauffmann, Guinevere</style></author><author><style face="normal" font="default" size="100%">Kazin, Eyal</style></author><author><style face="normal" font="default" size="100%">Kirkby, David</style></author><author><style face="normal" font="default" size="100%">Klaene, Mark A.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kneib, Jean-Paul</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Koesterke, Lars</style></author><author><style face="normal" font="default" size="100%">Kollmeier, Juna A.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lang, Dustin</style></author><author><style face="normal" font="default" size="100%">Lawler, James E.</style></author><author><style face="normal" font="default" size="100%">Le Goff, Jean-Marc</style></author><author><style face="normal" font="default" size="100%">Lee, Brian L.</style></author><author><style face="normal" font="default" size="100%">Lee, Young Sun</style></author><author><style face="normal" font="default" size="100%">Leisenring, Jarron M.</style></author><author><style face="normal" font="default" size="100%">Lin, Yen-Ting</style></author><author><style face="normal" font="default" size="100%">Liu, Jian</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Lucatello, Sara</style></author><author><style face="normal" font="default" size="100%">Lundgren, Britt</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Ma, Bo</style></author><author><style face="normal" font="default" size="100%">Ma, Zhibo</style></author><author><style face="normal" font="default" size="100%">MacDonald, Nicholas</style></author><author><style face="normal" font="default" size="100%">Mack, Claude</style></author><author><style face="normal" font="default" size="100%">Mahadevan, Suvrath</style></author><author><style face="normal" font="default" size="100%">Maia, Marcio A. G.</style></author><author><style face="normal" font="default" size="100%">Majewski, Steven R.</style></author><author><style face="normal" font="default" size="100%">Makler, Martin</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Margala, Daniel</style></author><author><style face="normal" font="default" size="100%">Maseman, Paul</style></author><author><style face="normal" font="default" size="100%">Masters, Karen L.</style></author><author><style face="normal" font="default" size="100%">McBride, Cameron K.</style></author><author><style face="normal" font="default" size="100%">McDonald, Patrick</style></author><author><style face="normal" font="default" size="100%">McGreer, Ian D.</style></author><author><style face="normal" font="default" size="100%">McMahon, Richard G.</style></author><author><style face="normal" font="default" size="100%">Mena Requejo, Olga</style></author><author><style face="normal" font="default" size="100%">Ménard, Brice</style></author><author><style face="normal" font="default" size="100%">Miralda-Escudé, Jordi</style></author><author><style face="normal" font="default" size="100%">Morrison, Heather L.</style></author><author><style face="normal" font="default" size="100%">Mullally, Fergal</style></author><author><style face="normal" font="default" size="100%">Muna, Demitri</style></author><author><style face="normal" font="default" size="100%">Murayama, Hitoshi</style></author><author><style face="normal" font="default" size="100%">Myers, Adam D.</style></author><author><style face="normal" font="default" size="100%">Naugle, Tracy</style></author><author><style face="normal" font="default" size="100%">Fausti Neto, Angelo</style></author><author><style face="normal" font="default" size="100%">Cuong Nguyen, Duy</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nidever, David L.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Robert W.</style></author><author><style face="normal" font="default" size="100%">Ogando, Ricardo L. C.</style></author><author><style face="normal" font="default" size="100%">Olmstead, Matthew D.</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Paegert, Martin</style></author><author><style face="normal" font="default" size="100%">Palanque-Delabrouille, Nathalie</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Pandey, Parul</style></author><author><style face="normal" font="default" size="100%">Parejko, John K.</style></author><author><style face="normal" font="default" size="100%">Pâris, Isabelle</style></author><author><style face="normal" font="default" size="100%">Pellegrini, Paulo</style></author><author><style face="normal" font="default" size="100%">Pepper, Joshua</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Petitjean, Patrick</style></author><author><style face="normal" font="default" size="100%">Pfaffenberger, Robert</style></author><author><style face="normal" font="default" size="100%">Pforr, Janine</style></author><author><style face="normal" font="default" size="100%">Phleps, Stefanie</style></author><author><style face="normal" font="default" size="100%">Pichon, Christophe</style></author><author><style face="normal" font="default" size="100%">Pieri, Matthew M.</style></author><author><style face="normal" font="default" size="100%">Prada, Francisco</style></author><author><style face="normal" font="default" size="100%">Price-Whelan, Adrian M.</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Ramos, Beatriz H. F.</style></author><author><style face="normal" font="default" size="100%">Reid, I. Neill</style></author><author><style face="normal" font="default" size="100%">Reyle, Celine</style></author><author><style face="normal" font="default" size="100%">Rich, James</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rieke, George H.</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia J.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Robin, Annie C.</style></author><author><style face="normal" font="default" size="100%">Rocha-Pinto, Helio J.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Roe, Natalie A.</style></author><author><style face="normal" font="default" size="100%">Rollinde, Emmanuel</style></author><author><style face="normal" font="default" size="100%">Ross, Ashley J.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Rossetto, Bruno</style></author><author><style face="normal" font="default" size="100%">Sánchez, Ariel G.</style></author><author><style face="normal" font="default" size="100%">Santiago, Basilio</style></author><author><style face="normal" font="default" size="100%">Sayres, Conor</style></author><author><style face="normal" font="default" size="100%">Schiavon, Ricardo</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schlesinger, Katharine J.</style></author><author><style face="normal" font="default" size="100%">Schmidt, Sarah J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Sellgren, Kris</style></author><author><style face="normal" font="default" size="100%">Shelden, Alaina</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shetrone, Matthew</style></author><author><style face="normal" font="default" size="100%">Shu, Yiping</style></author><author><style face="normal" font="default" size="100%">Silverman, John D.</style></author><author><style face="normal" font="default" size="100%">Simmerer, Jennifer</style></author><author><style face="normal" font="default" size="100%">Simmons, Audrey E.</style></author><author><style face="normal" font="default" size="100%">Sivarani, Thirupathi</style></author><author><style face="normal" font="default" size="100%">Skrutskie, M. F.</style></author><author><style face="normal" font="default" size="100%">Slosar, Anže</style></author><author><style face="normal" font="default" size="100%">Smee, Stephen</style></author><author><style face="normal" font="default" size="100%">Smith, Verne V.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stassun, Keivan G.</style></author><author><style face="normal" font="default" size="100%">Steele, Oliver</style></author><author><style face="normal" font="default" size="100%">Steinmetz, Matthias</style></author><author><style face="normal" font="default" size="100%">Stockett, Mark H.</style></author><author><style face="normal" font="default" size="100%">Stollberg, Todd</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Tanaka, Masayuki</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Thomas, Daniel</style></author><author><style face="normal" font="default" size="100%">Tinker, Jeremy L.</style></author><author><style face="normal" font="default" size="100%">Tofflemire, Benjamin M.</style></author><author><style face="normal" font="default" size="100%">Tojeiro, Rita</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Vargas Magaña, Mariana</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Wan, Xiaoke</style></author><author><style face="normal" font="default" size="100%">Wang, Ji</style></author><author><style face="normal" font="default" size="100%">Weaver, Benjamin A.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilson, John C.</style></author><author><style face="normal" font="default" size="100%">Wisniewski, John P.</style></author><author><style face="normal" font="default" size="100%">Wood-Vasey, W. Michael</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yasuda, Naoki</style></author><author><style face="normal" font="default" size="100%">Yèche, Christophe</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Young, Erick</style></author><author><style face="normal" font="default" size="100%">Zasowski, Gail</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zhao, Bo</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS-III: Massive Spectroscopic Surveys of the Distant Universe, the Milky Way, and Extra-Solar Planetary Systems</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2011</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2011AJ....142...72E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">142</style></volume><pages><style face="normal" font="default" size="100%">72</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Building on the legacy of the Sloan Digital Sky Survey (SDSS-I and II),SDSS-III is a program of four spectroscopic surveys on three scientificthemes: dark energy and cosmological parameters, the history andstructure of the Milky Way, and the population of giant planets aroundother stars. In keeping with SDSS tradition, SDSS-III will provideregular public releases of all its data, beginning with SDSS DataRelease 8 (DR8), which was made public in 2011 January and includesSDSS-I and SDSS-II images and spectra reprocessed with the latestpipelines and calibrations produced for the SDSS-III investigations.This paper presents an overview of the four surveys that compriseSDSS-III. The Baryon Oscillation Spectroscopic Survey will measureredshifts of 1.5 million massive galaxies and Lyα forest spectraof 150,000 quasars, using the baryon acoustic oscillation feature oflarge-scale structure to obtain percent-level determinations of thedistance scale and Hubble expansion rate at z &amp;lt; 0.7 and at z ≈2.5. SEGUE-2, an already completed SDSS-III survey that is thecontinuation of the SDSS-II Sloan Extension for Galactic Understandingand Exploration (SEGUE), measured medium-resolution (R =λ/Δλ ≈ 1800) optical spectra of 118,000 stars ina variety of target categories, probing chemical evolution, stellarkinematics and substructure, and the mass profile of the dark matterhalo from the solar neighborhood to distances of 100 kpc. APOGEE, theApache Point Observatory Galactic Evolution Experiment, will obtainhigh-resolution (R ≈ 30,000), high signal-to-noise ratio (S/N &amp;gt;=100 per resolution element), H-band (1.51 μm &amp;lt; λ &amp;lt; 1.70μm) spectra of 10&lt;sup&gt;5&lt;/sup&gt; evolved, late-type stars, measuringseparate abundances for ~15 elements per star and creating the firsthigh-precision spectroscopic survey of all Galactic stellar populations(bulge, bar, disks, halo) with a uniform set of stellar tracers andspectral diagnostics. The Multi-object APO Radial Velocity ExoplanetLarge-area Survey (MARVELS) will monitor radial velocities of more than8000 FGK stars with the sensitivity and cadence (10-40 m s&lt;sup&gt;-1&lt;/sup&gt;,~24 visits per star) needed to detect giant planets with periods up totwo years, providing an unprecedented data set for understanding theformation and dynamical evolution of giant planet systems. As of 2011January, SDSS-III has obtained spectra of more than 240,000 galaxies,29,000 z &amp;gt;= 2.2 quasars, and 140,000 stars, including 74,000 velocitymeasurements of 2580 stars for MARVELS.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1101.1529</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Reid, Beth A.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Budavari, Tamas</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Spergel, David N.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Baryon acoustic oscillations in the Sloan Digital Sky Survey Data Release 7 galaxy sample</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2010</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010MNRAS.401.2148P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">401</style></volume><pages><style face="normal" font="default" size="100%">2148-2168</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The spectroscopic Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7)galaxy sample represents the final set of galaxies observed using theoriginal SDSS target selection criteria. We analyse the clustering ofgalaxies within this sample, including both the luminous red galaxy andmain samples, and also include the 2-degree Field Galaxy Redshift Surveydata. In total, this sample comprises 893319 galaxies over9100deg&lt;sup&gt;2&lt;/sup&gt;. Baryon acoustic oscillations (BAO) are observed inpower spectra measured for different slices in redshift; this allows usto constrain the distance-redshift relation at multiple epochs. Weachieve a distance measure at redshift z = 0.275, ofr&lt;sub&gt;s&lt;/sub&gt;(z&lt;sub&gt;d&lt;/sub&gt;)/D&lt;sub&gt;V&lt;/sub&gt;(0.275) = 0.1390 +/- 0.0037(2.7 per cent accuracy), where r&lt;sub&gt;s&lt;/sub&gt;(z&lt;sub&gt;d&lt;/sub&gt;) is thecomoving sound horizon at the baryon-drag epoch, D&lt;sub&gt;V&lt;/sub&gt;(z)≡ [(1 +z)&lt;sup&gt;2&lt;/sup&gt;D&lt;sup&gt;2&lt;/sup&gt;&lt;sub&gt;A&lt;/sub&gt;cz/H(z)]&lt;sup&gt;1/3&lt;/sup&gt;,D&lt;sub&gt;A&lt;/sub&gt;(z) is the angular diameter distance and H(z) is the Hubbleparameter. We find an almost independent constraint on the ratio ofdistances D&lt;sub&gt;V&lt;/sub&gt;(0.35)/D&lt;sub&gt;V&lt;/sub&gt;(0.2) = 1.736 +/- 0.065,which is consistent at the 1.1σ level with the best-fittingΛ cold dark matter model obtained when combining our z = 0.275distance constraint with the Wilkinson Microwave Anisotropy Probe 5-year(WMAP5) data. The offset is similar to that found in previous analysesof the SDSS DR5 sample, but the discrepancy is now of lowersignificance, a change caused by a revised error analysis and a changein the methodology adopted, as well as the addition of more data. UsingWMAP5 constraints on Ω&lt;sub&gt;b&lt;/sub&gt;h&lt;sup&gt;2&lt;/sup&gt; andΩ&lt;sub&gt;c&lt;/sub&gt;h&lt;sup&gt;2&lt;/sup&gt;, and combining our BAO distancemeasurements with those from the Union supernova sample, places a tightconstraint on Ω&lt;sub&gt;m&lt;/sub&gt; = 0.286 +/- 0.018 and H&lt;sub&gt;0&lt;/sub&gt; =68.2 +/- 2.2kms&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-1&lt;/sup&gt; that is robust to allowingΩ&lt;sub&gt;k&lt;/sub&gt; ≠ 0 and w ≠ -1. This result is independent ofthe behaviour of dark energy at redshifts greater than those probed bythe BAO and supernova measurements. Combining these data sets with thefull WMAP5 likelihood constraints provides tight constraints on bothΩ&lt;sub&gt;k&lt;/sub&gt; = -0.006 +/- 0.008 and w = -0.97 +/- 0.10 for aconstant dark energy equation of state.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0907.1660</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Reid, Beth A.</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Spergel, David N.</style></author><author><style face="normal" font="default" size="100%">Skibba, Ramin A.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Budavari, Tamas</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gott, J. Richard</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2010</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010MNRAS.404...60R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">404</style></volume><pages><style face="normal" font="default" size="100%">60-85</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the power spectrum of the reconstructed halo density fieldderived from a sample of luminous red galaxies (LRGs) from the SloanDigital Sky Survey (SDSS) Seventh Data Release (DR7). The halo powerspectrum has a direct connection to the underlying dark matter power fork &amp;lt;= 0.2hMpc&lt;sup&gt;-1&lt;/sup&gt;, well into the quasi-linear regime. Thisenables us to use a factor of ~8 more modes in the cosmological analysisthan an analysis with k&lt;sub&gt;max&lt;/sub&gt; = 0.1hMpc&lt;sup&gt;-1&lt;/sup&gt;, as wasadopted in the SDSS team analysis of the DR4 LRG sample. The observedhalo power spectrum for 0.02 &amp;lt; k &amp;lt; 0.2hMpc&lt;sup&gt;-1&lt;/sup&gt; is wellfitted by our model: χ&lt;sup&gt;2&lt;/sup&gt; = 39.6 for 40 degrees of freedomfor the best-fitting Λ cold dark matter (ΛCDM) model. Wefind Ω&lt;sub&gt;m&lt;/sub&gt;h&lt;sup&gt;2&lt;/sup&gt;(n&lt;sub&gt;s&lt;/sub&gt;/0.96)&lt;sup&gt;1.2&lt;/sup&gt;= 0.141&lt;sup&gt;+0.010&lt;/sup&gt;&lt;sub&gt;-0.012&lt;/sub&gt; for a power-law primordialpower spectrum with spectral index n&lt;sub&gt;s&lt;/sub&gt; andΩ&lt;sub&gt;b&lt;/sub&gt;h&lt;sup&gt;2&lt;/sup&gt; = 0.02265 fixed, consistent with cosmicmicrowave background measurements. The halo power spectrum alsoconstrains the ratio of the comoving sound horizon at the baryon-dragepoch to an effective distance to z = 0.35:r&lt;sub&gt;s&lt;/sub&gt;/D&lt;sub&gt;V&lt;/sub&gt;(0.35) =0.1097&lt;sup&gt;+0.0039&lt;/sup&gt;&lt;sub&gt;-0.0042&lt;/sub&gt;. Combining the halo powerspectrum measurement with the Wilkinson Microwave Anisotropy Probe(WMAP) 5 year results, for the flat ΛCDM model we findΩ&lt;sub&gt;m&lt;/sub&gt; = 0.289 +/- 0.019 and H&lt;sub&gt;0&lt;/sub&gt; = 69.4 +/-1.6kms&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-1&lt;/sup&gt;. Allowing for massive neutrinos inΛCDM, we find eV at the 95 per cent confidence level. If weinstead consider the effective number of relativistic speciesN&lt;sub&gt;eff&lt;/sub&gt; as a free parameter, we find N&lt;sub&gt;eff&lt;/sub&gt; =4.8&lt;sup&gt;+1.8&lt;/sup&gt;&lt;sub&gt;-1.7&lt;/sub&gt;. Combining also with the Kowalski etal. supernova sample, we find Ω&lt;sub&gt;tot&lt;/sub&gt; = 1.011 +/- 0.009and w = -0.99 +/- 0.11 for an open cosmology with constant dark energyequation of state w. The power spectrum and a module to calculate thelikelihoods are publicly available athttp://lambda.gsfc.nasa.gov/toolbox/lrgdr/.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0907.1659</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Rujopakarn, Wiphu</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Rieke, George H.</style></author><author><style face="normal" font="default" size="100%">Papovich, Casey</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Moustakas, John</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia J.</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, Peter</style></author><author><style face="normal" font="default" size="100%">Murray, Steve S.</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Le Floc'h, Emeric</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Evolution of the Star Formation Rate of Galaxies at 0.0 &lt;= z &lt;= 1.2</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2010</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010ApJ...718.1171R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">718</style></volume><pages><style face="normal" font="default" size="100%">1171-1185</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the 24 μm rest-frame luminosity function (LF) ofstar-forming galaxies in the redshift range 0.0 &amp;lt;= z &amp;lt;= 0.6constructed from 4047 spectroscopic redshifts from the AGN and GalaxyEvolution Survey of 24 μm selected sources in the Boötes fieldof the NOAO Deep Wide-Field Survey. This sample provides the bestavailable combination of large area (9 deg&lt;sup&gt;2&lt;/sup&gt;), depth, andstatistically complete spectroscopic observations, allowing us to probethe evolution of the 24 μm LF of galaxies at low and intermediateredshifts while minimizing the effects of cosmic variance. In order touse the observed 24 μm luminosity as a tracer for star formation,active galactic nuclei (AGNs) that could contribute significantly at 24μm are identified and excluded from our star-forming galaxy samplebased on their mid-IR spectral energy distributions or the detection ofX-ray emission. Optical emission line diagnostics are considered for AGNidentification, but we find that 24 μm emission from opticallyselected AGNs is usually from star-forming activity and therefore shouldnot be excluded. The evolution of the 24 μm LF of star-forminggalaxies for redshifts of z &amp;lt;= 0.65 is consistent with a pureluminosity evolution where the characteristic 24 μm luminosityevolves as (1 + z)&lt;sup&gt;3.8±0.3&lt;/sup&gt;. We extend our evolutionarystudy to encompass 0.0 &amp;lt;= z &amp;lt;= 1.2 by combining our data with thatof the Far-Infrared Deep Extragalactic Legacy Survey. Over this entireredshift range, the evolution of the characteristic 24 μm luminosityis described by a slightly shallower power law of (1 +z)&lt;sup&gt;3.4±0.2&lt;/sup&gt;. We find a local star formation rate densityof (1.09 ± 0.21) × 10&lt;sup&gt;-2&lt;/sup&gt; M &lt;sub&gt;sun&lt;/sub&gt;yr&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;, and that it evolves as (1 +z)&lt;sup&gt;3.5±0.2&lt;/sup&gt; over 0.0 &amp;lt;= z &amp;lt;= 1.2. These estimatesare in good agreement with the rates using optical and UV fluxescorrected for the effects of intrinsic extinction in the observedsources. This agreement confirms that star formation at z &amp;lt;~ 1.2 isrobustly traced by 24 μm observations and that it largely occurs inobscured regions of galaxies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1006.4359</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eckel, Jonathan</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Mehta, Kushal</style></author><author><style face="normal" font="default" size="100%">Metchnik, Marc</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Pinto, Phillip</style></author><author><style face="normal" font="default" size="100%">Takahashi, Ryuichi</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Xu, Xiaoying</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">High-precision Predictions for the Acoustic Scale in the Nonlinear Regime</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 201</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010ApJ...720.1650S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">720</style></volume><pages><style face="normal" font="default" size="100%">1650-1667</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We measure shifts of the acoustic scale due to nonlinear growth andredshift distortions to a high precision using a very large volume ofhigh-force-resolution simulations. We compare results from various setsof simulations that differ in their force, volume, and mass resolution.We find a consistency within 1.5σ for shift values from differentsimulations and derive shift α(z) - 1 = (0.300 ± 0.015)&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0910.5005</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Xu, X.</style></author><author><style face="normal" font="default" size="100%">White, M.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, N.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Eckel, J.</style></author><author><style face="normal" font="default" size="100%">Mehta, K.</style></author><author><style face="normal" font="default" size="100%">Metchnik, M.</style></author><author><style face="normal" font="default" size="100%">Pinto, P.</style></author><author><style face="normal" font="default" size="100%">Seo, H.-J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A New Statistic for Analyzing Baryon Acoustic Oscillations</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2010</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010ApJ...718.1224X</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">718</style></volume><pages><style face="normal" font="default" size="100%">1224-1234</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We introduce a new statistic ω&lt;sub&gt;ell&lt;/sub&gt;(r&lt;sub&gt;s&lt;/sub&gt; ) formeasuring and analyzing large-scale structure and particularly thebaryon acoustic oscillations. ω&lt;sub&gt;ell&lt;/sub&gt;(r&lt;sub&gt;s&lt;/sub&gt; ) is aband-filtered, configuration space statistic that is easily implementedand has advantages over the traditional power spectrum and correlationfunction estimators. Unlike these estimators,ω&lt;sub&gt;ell&lt;/sub&gt;(r&lt;sub&gt;s&lt;/sub&gt; ) can localize most of the acousticinformation into a single dip at the acoustic scale while avoidingsensitivity to the poorly constrained large-scale power (i.e., theintegral constraint) through the use of a localized and compensatedfilter. It is also sensitive to anisotropic clustering through paircounting and does not require any binning of data. We measure the shiftin the acoustic peak due to nonlinear effects using the monopoleω&lt;sub&gt;0&lt;/sub&gt;(r&lt;sub&gt;s&lt;/sub&gt; ) derived from subsampled dark matter(DM) catalogs as well as from mock galaxy catalogs created via halooccupation distribution modeling. All of these are drawn from 44realizations of 1024&lt;sup&gt;3&lt;/sup&gt; particle DM simulations in a 1 h&lt;sup&gt;-1&lt;/sup&gt; Gpc box at z = 1. We compare these shifts with thoseobtained from the power spectrum and conclude that the results agree. Wetherefore expect that distance measurements obtained fromω&lt;sub&gt;0&lt;/sub&gt;(r&lt;sub&gt;s&lt;/sub&gt; ) and P(k) will be consistent witheach other. We also show that it is possible to extract the same amountof acoustic information by fitting over a finite range using eitherω&lt;sub&gt;0&lt;/sub&gt;(r&lt;sub&gt;s&lt;/sub&gt; ) or P(k) derived from equal volumesurveys.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1001.2324</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Boroson, Todd A.</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Shen, Yue</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Krawczyk, Coleman M.</style></author><author><style face="normal" font="default" size="100%">Thakar, Anirudda R.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hibon, Pascale</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Lee, Myung Gyoon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Elena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Oravetz, Dan</style></author><author><style face="normal" font="default" size="100%">Pan, K.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Price, Ted N.</style></author><author><style face="normal" font="default" size="100%">Saxe, David H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Simmons, Audry</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark U.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey Quasar Catalog. V. Seventh Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2010</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010AJ....139.2360S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">139</style></volume><pages><style face="normal" font="default" size="100%">2360-2373</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the fifth edition of the Sloan Digital Sky Survey (SDSS)Quasar Catalog, which is based upon the SDSS Seventh Data Release. Thecatalog, which contains 105,783 spectroscopically confirmed quasars,represents the conclusion of the SDSS-I and SDSS-II quasar survey. Thecatalog consists of the SDSS objects that have luminosities larger thanM&lt;sub&gt;i&lt;/sub&gt; = -22.0 (in a cosmology with H &lt;sub&gt;0&lt;/sub&gt; = 70 kms&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;, Ω&lt;sub&gt; M &lt;/sub&gt; = 0.3, andΩ&lt;sub&gt;Λ&lt;/sub&gt; = 0.7), have at least one emission line withFWHM larger than 1000 km s&lt;sup&gt;-1&lt;/sup&gt; or have interesting/complexabsorption features, are fainter than i ≈ 15.0, and have highlyreliable redshifts. The catalog covers an area of ≈9380deg&lt;sup&gt;2&lt;/sup&gt;. The quasar redshifts range from 0.065 to 5.46, with amedian value of 1.49; the catalog includes 1248 quasars at redshiftsgreater than 4, of which 56 are at redshifts greater than 5. The catalogcontains 9210 quasars with i &amp;lt; 18; slightly over half of the entrieshave i &amp;lt; 19. For each object the catalog presents positions accurateto better than 0farcs1 rms per coordinate, five-band (ugriz) CCD-basedphotometry with typical accuracy of 0.03 mag, and information on themorphology and selection method. The catalog also contains radio,near-infrared, and X-ray emission properties of the quasars, whenavailable, from other large-area surveys. The calibrated digital spectracover the wavelength region 3800-9200 Å at a spectral resolutionof ~= 2000; the spectra can be retrieved from the SDSS public database&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1004.1167</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Yang, Yujin</style></author><author><style face="normal" font="default" size="100%">Zabludoff, Ann</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Davé, Romeel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Strong Field-to-field Variation of Lyα Nebulae Populations at z ~= 2.3</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2010</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2010ApJ...719.1654Y</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">719</style></volume><pages><style face="normal" font="default" size="100%">1654-1671</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Understanding the nature of distant Lyα nebulae, aka &quot;blobs,&quot; andconnecting them to their present-day descendants requires constrainingtheir number density, clustering, and large-scale environment. Tomeasure these basic quantities, we conduct a deep narrowband imagingsurvey in four different fields, Chandra Deep Field South (CDFS),Chandra Deep Field North (CDFN), and two COSMOS subfields, for a totalsurvey area of 1.2 deg&lt;sup&gt;2&lt;/sup&gt;. We discover 25 blobs at z = 2.3 withLyα luminosities of L &lt;sub&gt;Lyα&lt;/sub&gt;= (0.7-8) ×10&lt;sup&gt;43&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and isophotal areas of A&lt;sub&gt;iso&lt;/sub&gt; = 10-60 sq arcsec. The transition from compact Lyαemitters (LAEs; A &lt;sub&gt;iso&lt;/sub&gt; ~ a few sq arcsec) to extendedLyα blobs (A &lt;sub&gt;iso&lt;/sub&gt; &amp;gt; 10 sq arcsec) is continuous,suggesting a single family perhaps governed by similar emissionmechanisms. Surprisingly, most blobs (16/25) are in one survey field,the CDFS. The six brightest, largest blobs with L &lt;sub&gt;Lyα&lt;/sub&gt;gsim 1.5×10&lt;sup&gt;43&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and A &lt;sub&gt;iso&lt;/sub&gt;&amp;gt; 16 sq arcsec lie only in the CDFS. These large, bright blobs have a&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:1008.2776</style></custom3><reprint-edition><style face="normal" font="default" size="100%">structures.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Yang, Yujin</style></author><author><style face="normal" font="default" size="100%">Zabludoff, Ann</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Davé, Romeel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Extended Lyα Nebulae at z sime 2.3: An Extremely Rare and Strongly Clustered Population?</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...693.1579Y</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">693</style></volume><pages><style face="normal" font="default" size="100%">1579-1587</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;To obtain an unbiased sample of bright Lyα blobs (L_{Lyα}≳ 10^{43} erg s&lt;sup&gt;-1&lt;/sup&gt;), we have undertaken a blind,wide-field, narrowband imaging survey in the National Optical AstronomyObservatory Deep Wide Field Survey Boötes field with the StewardBok 2.3 m telescope. After searching over 4.82 deg&lt;sup&gt;2&lt;/sup&gt; at z =2.3, we discover four Lyα blobs with L_{Lyα} = 1.6-5.3× 10&lt;sup&gt;43&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, isophotal areas of 28-57⊓⊔, and broad Lyα line profiles (Δv = 900-1250km  s&lt;sup&gt;-1&lt;/sup&gt;). In contrast with the extended Lyα halosassociated with high-z radio galaxies, none of our four blobs areradio-loud. The X-ray luminosities and optical spectra of these blobsare diverse. Two blobs (3 and 4) are X-ray detected with L&lt;sub&gt;X&lt;/sub&gt;(2-7 keV) = 2-4 × 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and havebroad optical emission lines (C IV) characteristic of active galactic&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0811.3446</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Zheng, Zheng</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Jing, Y. P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Halo Occupation Distribution Modeling of Clustering of Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...707..554Z</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">707</style></volume><pages><style face="normal" font="default" size="100%">554-572</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We perform halo occupation distribution (HOD) modeling to interpretsmall-scale and intermediate-scale clustering of 35,000 luminousearly-type galaxies and their cross-correlation with a reference imagingsample of normal L &lt;sub&gt;*&lt;/sub&gt; galaxies in the Sloan Digital SkySurvey. The modeling results show that most of these luminous redgalaxies (LRGs) are central galaxies residing in massive halos oftypical mass M~ a few times 10&lt;sup&gt;13&lt;/sup&gt;-10&lt;sup&gt;14&lt;/sup&gt; h&lt;sup&gt;-1&lt;/sup&gt; M &lt;sub&gt;sun&lt;/sub&gt;, while a few percent of them have to besatellites within halos in order to produce the strong auto-correlationsexhibited on smaller scales. The mean luminosity L&lt;sub&gt;c&lt;/sub&gt; ofcentral LRGs increases with the host halo mass, with a rough scalingrelation of L&lt;sub&gt;c&lt;/sub&gt; vprop M &lt;sup&gt;0.5&lt;/sup&gt;. The halo mass requiredto host on average one satellite LRG above a luminosity threshold isfound to be about 10 times higher than that required to host a centralLRG above the same threshold. We find that in massive halos thedistribution of L &lt;sub&gt;*&lt;/sub&gt; galaxies roughly follows that of the darkmatter and their mean occupation number scales with halo mass as M&lt;sup&gt;1.5&lt;/sup&gt;. The HOD modeling results also allow for an intuitiveunderstanding of the scale-dependent luminosity dependence of thecross-correlation between LRGs and L &lt;sub&gt;*&lt;/sub&gt; galaxies. Constraintson the LRG HOD provide tests for models of formation and evolution ofmassive galaxies, and they are also useful for cosmological parameterinvestigations. In one of the appendices, we provide LRG HOD parameterswith dependence on cosmology inferred from modeling the two-pointauto-correlation functions of LRGs.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0809.1868</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hickox, Ryan C.</style></author><author><style face="normal" font="default" size="100%">Jones, Christine</style></author><author><style face="normal" font="default" size="100%">Forman, William R.</style></author><author><style face="normal" font="default" size="100%">Murray, Stephen S.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Stern, Daniel</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, Peter R.</style></author><author><style face="normal" font="default" size="100%">Gorjian, Varoujan</style></author><author><style face="normal" font="default" size="100%">Brodwin, Mark</style></author><author><style face="normal" font="default" size="100%">Narayan, Ramesh</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Kenter, Almus</style></author><author><style face="normal" font="default" size="100%">Caldwell, Nelson</style></author><author><style face="normal" font="default" size="100%">Anderson, Michael E.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Host Galaxies, Clustering, Eddington Ratios, and Evolution of Radio, X-Ray, and Infrared-Selected AGNs</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...696..891H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">696</style></volume><pages><style face="normal" font="default" size="100%">891-919</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We explore the connection between different classes of active galacticnuclei (AGNs) and the evolution of their host galaxies, by deriving hostgalaxy properties, clustering, and Eddington ratios of AGNs selected inthe radio, X-ray, and infrared (IR) wavebands. We study a sample of 585AGNs at 0.25 &amp;lt; z &amp;lt; 0.8 using redshifts from the AGN and GalaxyEvolution Survey (AGES). We select AGNs with observations in the radioat 1.4 GHz from the Westerbork Synthesis Radio Telescope, X-rays fromthe Chandra XBoötes Survey, and mid-IR from the Spitzer IRACShallow Survey. The radio, X-ray, and IR AGN samples show only modestoverlap, indicating that to the flux limits of the survey, theyrepresent largely distinct classes of AGNs. We derive host galaxy colorsand luminosities, as well as Eddington ratios, for obscured or opticallyfaint AGNs. We also measure the two-point cross-correlation between AGNsand galaxies on scales of 0.3-10 h &lt;sup&gt;-1&lt;/sup&gt; Mpc, and derive typicaldark matter halo masses. We find that: (1) radio AGNs are mainly foundin luminous red sequence galaxies, are strongly clustered (with M&lt;sub&gt;halo&lt;/sub&gt; ~ 3 × 10&lt;sup&gt;13&lt;/sup&gt; h &lt;sup&gt;-1&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;), and have very low Eddington ratios λ lsim10&lt;sup&gt;-3&lt;/sup&gt; (2) X-ray-selected AGNs are preferentially found ingalaxies that lie in the &quot;green valley&quot; of color-magnitude space and areclustered similar to the typical AGES galaxies (M &lt;sub&gt;halo&lt;/sub&gt; ~10&lt;sup&gt;13&lt;/sup&gt; h &lt;sup&gt;-1&lt;/sup&gt; M &lt;sub&gt;sun&lt;/sub&gt;), with 10&lt;sup&gt;-3&lt;/sup&gt;lsim λ lsim 1; (3) IR AGNs reside in slightly bluer, slightlyless luminous galaxies than X-ray AGNs, are weakly clustered (M&lt;sub&gt;halo&lt;/sub&gt; lsim 10&lt;sup&gt;12&lt;/sup&gt; h &lt;sup&gt;-1&lt;/sup&gt; M &lt;sub&gt;sun&lt;/sub&gt;),and have λ&amp;gt;10&lt;sup&gt;-2&lt;/sup&gt;. We interpret these results interms of a simple model of AGN and galaxy evolution, whereby a &quot;quasar&quot;phase and the growth of the stellar bulge occurs when a galaxy's darkmatter halo reaches a critical mass between ~10&lt;sup&gt;12&lt;/sup&gt; and10&lt;sup&gt;13&lt;/sup&gt; M &lt;sub&gt;sun&lt;/sub&gt;. After this event, star formationceases and AGN accretion shifts from radiatively efficient (optical- andIR-bright) to radiatively inefficient (optically faint, radio-bright)modes.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0901.4121</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Dai, X.</style></author><author><style face="normal" font="default" size="100%">Assef, R. J.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Brodwin, M.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Dey, A.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, A. H.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Jones, C.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Mid-Infrared Galaxy Luminosity Functions from the AGN and Galaxy Evolution Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...697..506D</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">697</style></volume><pages><style face="normal" font="default" size="100%">506-521</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present galaxy luminosity functions at 3.6, 4.5, 5.8, and 8.0 μmmeasured by combining photometry from the IRAC Shallow Survey withredshifts from the AGN and Galaxy Evolution Survey (AGES) of the NOAODeep Wide-Field Survey Boötes field. The well defined IRAC samplescontain 3800-5800 galaxies for the 3.6-8.0 μm bands withspectroscopic redshifts and z &amp;lt; 0.6. We obtained relatively completeluminosity functions in the local redshift bin of z &amp;lt; 0.2 for allfour IRAC channels that are well fitted by Schechter functions. Afteranalyzing the samples for the whole redshift range, we found significantevolution in the luminosity functions for all four IRAC channels thatcan be fitted as an evolution in M &lt;sub&gt;*&lt;/sub&gt; with redshift, ΔM&lt;sub&gt;*&lt;/sub&gt; = Qz. While we measured Q = 1.2 ± 0.4 and 1.1± 0.4 in the 3.6 and 4.5 μm bands consistent with thepredictions from a passively evolving population, we obtained Q = 1.8± 1.1 in the 8.0 μm band consistent with other evolving starformation rate estimates. We compared our luminosity functions with thepredictions of semianalytical galaxy formation and found the bestagreement at 3.6 and 4.5 μm, rough agreement at 8.0 μm, and alarge mismatch at 5.8 μm. These models also predicted a comparableQ-value to our luminosity functions at 8.0 μm, but predicted smallervalues at 3.6 and 4.5 μm. We also measured the luminosity functionsseparately for early- and late-type galaxies. While the luminosityfunctions of late-type galaxies resemble those for the total population,the luminosity functions of early-type galaxies in the 3.6 and 4.5 μmbands indicate deviations from the passive evolution model, especiallyfrom the measured flat luminosity density evolution. Combining ourestimates with other measurements in the literature, we found 53&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0902.2812</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, Rodger I.</style></author><author><style face="normal" font="default" size="100%">Bechtold, Jill</style></author><author><style face="normal" font="default" size="100%">Black, John H.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Kennicutt, Robert C.</style></author><author><style face="normal" font="default" size="100%">Martins, Carlos</style></author><author><style face="normal" font="default" size="100%">Prochaska, J. Xavier</style></author><author><style face="normal" font="default" size="100%">Shirley, Yancey L.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">An Observational Determination of the Proton to Electron Mass Ratio in the Early Universe</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...703.1648T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">703</style></volume><pages><style face="normal" font="default" size="100%">1648-1662</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;In an effort to resolve the discrepancy between two measurements of thefundamental constant μ, the proton to electron mass ratio, at earlytimes in the universe we reanalyze the same data used in the earlierstudies. Our analysis of the molecular hydrogen absorption lines inarchival Very Large Telescope/Ultraviolet and Visible EchelleSpectrometer (UVES) spectra of the damped Lyman alpha systems in thequasi-stellar objects Q0347-383 and Q0405-443 yields a combinedmeasurement of a Δμ/μ value of (-7 ± 8) ×10&lt;sup&gt;-6&lt;/sup&gt;, consistent with no change in the value of μ over atime span of 11.5 Gyr. Here, we define Δμ as (μ&lt;sub&gt; z&lt;/sub&gt; - μ&lt;sub&gt;0&lt;/sub&gt;) where μ&lt;sub&gt; z &lt;/sub&gt; is the value of μat a redshift of z and μ&lt;sub&gt;0&lt;/sub&gt; is the present-day value. Ournull result is consistent with the recent measurements of King et al.,Δμ/μ = (2.6 ± 3.0) × 10&lt;sup&gt;-6&lt;/sup&gt;, andinconsistent with the positive detection of a change in μ by Reinholdet al. Both of the previous studies and this study are based on the samedata but with differing analysis methods. Improvements in the wavelengthcalibration over the UVES pipeline calibration is a key element in bothof the null results. This leads to the conclusion that the fundamentalconstant μ is unchanged to an accuracy of 10&lt;sup&gt;-5&lt;/sup&gt; over the&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0907.4392</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Abazajian, Kevork N.</style></author><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">An, Deokkeun</style></author><author><style face="normal" font="default" size="100%">Anderson, Kurt S. J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bailer-Jones, C. A. L.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Bassett, Bruce A.</style></author><author><style face="normal" font="default" size="100%">Becker, Andrew C.</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Bell, Eric F.</style></author><author><style face="normal" font="default" size="100%">Belokurov, Vasily</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Berman, Eileen F.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Bickerton, Steven J.</style></author><author><style face="normal" font="default" size="100%">Bizyaev, Dmitry</style></author><author><style face="normal" font="default" size="100%">Blakeslee, John P.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinchmann, Jarle</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carey, Larry N.</style></author><author><style face="normal" font="default" size="100%">Carliles, Samuel</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Cinabro, David</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Cunha, Carlos E.</style></author><author><style face="normal" font="default" size="100%">Czarapata, Paul C.</style></author><author><style face="normal" font="default" size="100%">Davenport, James R. A.</style></author><author><style face="normal" font="default" size="100%">de Haas, Ernst</style></author><author><style face="normal" font="default" size="100%">Dilday, Ben</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Evans, N. W.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gänsicke, Boris T.</style></author><author><style face="normal" font="default" size="100%">Gates, Evalyn</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Gilmore, G.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, Belinda</style></author><author><style face="normal" font="default" size="100%">Gonzalez, Carlos F.</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Györy, Zsuzsanna</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Harding, Paul</style></author><author><style face="normal" font="default" size="100%">Harris, Frederick H.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hayes, Jeffrey J. E.</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hoblitt, J.</style></author><author><style face="normal" font="default" size="100%">Hogan, Craig J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Hyde, Joseph B.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Takashi</style></author><author><style face="normal" font="default" size="100%">Im, Myungshin</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Jiang, Linhua</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kessler, R.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Konishi, Kohki</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Kuropatkin, Nikolay</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lebedeva, Svetlana</style></author><author><style face="normal" font="default" size="100%">Lee, Myung Gyoon</style></author><author><style face="normal" font="default" size="100%">Lee, Young Sun</style></author><author><style face="normal" font="default" size="100%">French Leger, R.</style></author><author><style face="normal" font="default" size="100%">Lépine, Sébastien</style></author><author><style face="normal" font="default" size="100%">Li, Nolan</style></author><author><style face="normal" font="default" size="100%">Lima, Marcos</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Magnier, Eugene</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Olena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Marriner, John P.</style></author><author><style face="normal" font="default" size="100%">Martínez-Delgado, David</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Morrison, Heather L.</style></author><author><style face="normal" font="default" size="100%">Mullally, Fergal</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Murphy, Tara</style></author><author><style face="normal" font="default" size="100%">Nash, Thomas</style></author><author><style face="normal" font="default" size="100%">Nebot, Ada</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Oravetz, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Park, Changbom</style></author><author><style face="normal" font="default" size="100%">Pauls, George</style></author><author><style face="normal" font="default" size="100%">Peoples, John, Jr.</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Pourbaix, Dimitri</style></author><author><style face="normal" font="default" size="100%">Price, Paul A.</style></author><author><style face="normal" font="default" size="100%">Purger, Norbert</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Re Fiorentin, Paola</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Riess, Adam G.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Sako, Masao</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scholz, Ralf-Dieter</style></author><author><style face="normal" font="default" size="100%">Schreiber, Matthias R.</style></author><author><style face="normal" font="default" size="100%">Schwope, Axel D.</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sesar, Branimir</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Sibley, Valena C.</style></author><author><style face="normal" font="default" size="100%">Simmons, A. E.</style></author><author><style face="normal" font="default" size="100%">Sivarani, Thirupathi</style></author><author><style face="normal" font="default" size="100%">Allyn Smith, J.</style></author><author><style face="normal" font="default" size="100%">Smith, Martin C.</style></author><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Steinmetz, Matthias</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Suto, Yasushi</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Tanaka, Masayuki</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Teodoro, Luis F. A.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vidrih, S.</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Wadadekar, Yogesh</style></author><author><style face="normal" font="default" size="100%">Watters, Shannon</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilhite, Brian C.</style></author><author><style face="normal" font="default" size="100%">Wonders, Alainna C.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zibetti, Stefano</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Seventh Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJS..182..543A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">182</style></volume><pages><style face="normal" font="default" size="100%">543-558</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper describes the Seventh Data Release of the Sloan Digital SkySurvey (SDSS), marking the completion of the original goals of the SDSSand the end of the phase known as SDSS-II. It includes 11,663deg&lt;sup&gt;2&lt;/sup&gt; of imaging data, with most of the ~2000 deg&lt;sup&gt;2&lt;/sup&gt;increment over the previous data release lying in regions of lowGalactic latitude. The catalog contains five-band photometry for 357million distinct objects. The survey also includes repeat photometry ona 120° long, 2fdg5 wide stripe along the celestial equator in theSouthern Galactic Cap, with some regions covered by as many as 90individual imaging runs. We include a co-addition of the best of thesedata, going roughly 2 mag fainter than the main survey over 250deg&lt;sup&gt;2&lt;/sup&gt;. The survey has completed spectroscopy over 9380deg&lt;sup&gt;2&lt;/sup&gt; the spectroscopy is now complete over a large contiguousarea of the Northern Galactic Cap, closing the gap that was present inprevious data releases. There are over 1.6 million spectra in total,including 930,000 galaxies, 120,000 quasars, and 460,000 stars. The datarelease includes improved stellar photometry at low Galactic latitude.The astrometry has all been recalibrated with the second version of theUSNO CCD Astrograph Catalog, reducing the rms statistical errors at thebright end to 45 milliarcseconds per coordinate. We further quantify asystematic error in bright galaxy photometry due to poor skydetermination; this problem is less severe than previously reported forthe majority of galaxies. Finally, we describe a series of improvementsto the spectroscopic reductions, including better flat fielding andimproved wavelength calibration at the blue end, better processing ofobjects with extremely strong narrow emission lines, and an improveddetermination of stellar metallicities.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0812.0649</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ashby, M. L. N.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author><author><style face="normal" font="default" size="100%">Brodwin, M.</style></author><author><style face="normal" font="default" size="100%">R Griffith</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P.</style></author><author><style face="normal" font="default" size="100%">Kozłowski, S.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Bock, J. J.</style></author><author><style face="normal" font="default" size="100%">Borys, C.</style></author><author><style face="normal" font="default" size="100%">Brand, K.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Cool, R.</style></author><author><style face="normal" font="default" size="100%">Cooray, A.</style></author><author><style face="normal" font="default" size="100%">Croft, S.</style></author><author><style face="normal" font="default" size="100%">Dey, A.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, A. H.</style></author><author><style face="normal" font="default" size="100%">Gorjian, V.</style></author><author><style face="normal" font="default" size="100%">Grogin, N. A.</style></author><author><style face="normal" font="default" size="100%">Ivison, R. J.</style></author><author><style face="normal" font="default" size="100%">Jacob, J.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Mainzer, A.</style></author><author><style face="normal" font="default" size="100%">Moustakas, L. A.</style></author><author><style face="normal" font="default" size="100%">Röttgering, H. J. A.</style></author><author><style face="normal" font="default" size="100%">Seymour, N.</style></author><author><style face="normal" font="default" size="100%">Smith, H. A.</style></author><author><style face="normal" font="default" size="100%">Stanford, S. A.</style></author><author><style face="normal" font="default" size="100%">Stauffer, J. R.</style></author><author><style face="normal" font="default" size="100%">Sullivan, I.</style></author><author><style face="normal" font="default" size="100%">van Breugel, W.</style></author><author><style face="normal" font="default" size="100%">Willner, S. P.</style></author><author><style face="normal" font="default" size="100%">Wright, E. L.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Spitzer Deep, Wide-field Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...701..428A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">701</style></volume><pages><style face="normal" font="default" size="100%">428-453</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infraredsurvey of 10 deg&lt;sup&gt;2&lt;/sup&gt; in the Boötes field of the NOAO DeepWide-Field Survey using the IRAC instrument on the Spitzer SpaceTelescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a uniqueposition in the area-depth survey space defined by other Spitzersurveys. The four epochs that make up SDWFS permit—for the firsttime—the selection of infrared-variable and high proper motionobjects over a wide field on timescales of years. Because of its largesurvey volume, SDWFS is sensitive to galaxies out to z ~ 3 withrelatively little impact from cosmic variance for all but the richestsystems. The SDWFS data sets will thus be especially useful forcharacterizing galaxy evolution beyond z ~ 1.5. This paper explains theSDWFS observing strategy and data processing, presents the SDWFS mosaicsand source catalogs, and discusses some early scientific findings. Thepublicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and0.96 × 10&lt;sup&gt;5&lt;/sup&gt; distinct sources detected to the average5σ, 4''-diameter, aperture-corrected limits of 19.77, 18.83,16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0 μm, respectively.The SDWFS number counts and color-color distribution are consistent withother, earlier Spitzer surveys. At the 6 minute integration time of the&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0906.0024</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Watson, Casey R.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Forman, William R.</style></author><author><style face="normal" font="default" size="100%">Hickox, Ryan C.</style></author><author><style face="normal" font="default" size="100%">Jones, Christine J.</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Brand, Kate</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Kenter, Almus T.</style></author><author><style face="normal" font="default" size="100%">Murray, Steve S.</style></author><author><style face="normal" font="default" size="100%">Vikhlinin, Alexey</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Fazio, Giovani G.</style></author><author><style face="normal" font="default" size="100%">Green, Paul J.</style></author><author><style face="normal" font="default" size="100%">McNamara, Brian R.</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia</style></author><author><style face="normal" font="default" size="100%">Shields, Joseph C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Star Formation and Nuclear Accretion Histories of Normal Galaxies in the Ages Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2009</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2009</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2009ApJ...696.2206W</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">696</style></volume><pages><style face="normal" font="default" size="100%">2206-2219</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We combine IR, optical, and X-ray data from the overlapping, 9.3deg&lt;sup&gt;2&lt;/sup&gt; NOAO Deep Wide-Field Survey, AGN and Galaxy EvolutionSurvey (AGES), and XBoötes Survey to measure the X-ray evolution of6146 normal galaxies as a function of absolute optical luminosity,redshift, and spectral type over the largely unexplored redshift range0.1 lsim z lsim 0.5. Because only the closest or brightest of thegalaxies are individually detected in X-rays, we use a stacking analysisto determine the mean properties of the sample. Our results suggest thatX-ray emission from spectroscopically late-type galaxies is dominated bystar formation, while that from early-type galaxies is dominated by acombination of hot gas and active galactic nucleus (AGN) emission. Wefind that the mean star formation and supermassive black hole accretionrate densities evolve like ~(1 + z)&lt;sup&gt;3±1&lt;/sup&gt;, in agreementwith the trends found for samples of bright, individually detectablestarburst galaxies and AGN. Our work also corroborates the results ofmany previous stacking analyses of faint source populations, withimproved statistics.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0903.2219</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Angel, Roger</style></author><author><style face="normal" font="default" size="100%">Worden, Simon P.</style></author><author><style face="normal" font="default" size="100%">Borra, Ermanno F.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Foing, Bernard</style></author><author><style face="normal" font="default" size="100%">Hickson, Paul</style></author><author><style face="normal" font="default" size="100%">Josset, Jean-Luc</style></author><author><style face="normal" font="default" size="100%">Ma, Ki Bui</style></author><author><style face="normal" font="default" size="100%">Seddiki, Omar</style></author><author><style face="normal" font="default" size="100%">Sivanandam, Suresh</style></author><author><style face="normal" font="default" size="100%">Thibault, Simon</style></author><author><style face="normal" font="default" size="100%">van Susante, Paul</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Cryogenic Liquid-Mirror Telescope on the Moon to Study the Early Universe</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...680.1582A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">680</style></volume><pages><style face="normal" font="default" size="100%">1582-1594</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We have studied the feasibility and scientific potential of zenithobserving liquid-mirror telescopes having 20-100 m diameters located onthe Moon. They would carry out deep infrared surveys to study thedistant universe and follow up discoveries made with the 6 m James WebbSpace Telescope (JWST), with more detailed images and spectroscopicstudies. They could detect objects 100 times fainter than JWST,observing the first high-redshift stars in the early universe and theirassembly into galaxies. We explored the scientific opportunities, keytechnologies, and optimum location of such telescopes. We havedemonstrated critical technologies. For example, the primary mirrorwould necessitate a high-reflectivity liquid that does not evaporate inthe lunar vacuum and remains liquid at less than 100 K. We have made acrucial demonstration by successfully coating an ionic liquid that hasnegligible vapor pressure. We also successfully experimented with aliquid mirror spinning on a superconducting bearing, as will be neededfor the cryogenic, vacuum environment of the telescope. We haveinvestigated issues related to lunar locations, concluding thatlocations within a few kilometers of a pole are ideal for deep sky coverand long integration times. We have located ridges and crater rimswithin 0.5° of the north pole that are illuminated for at least somesun angles during lunar winter, providing power and temperature control.We also have identified potential problems, like lunar dust. Issuesraised by our preliminary study demand additional in-depth analyses.These issues must be fully examined as part of a scientific debate thatwe hope to start with the present article.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0806.2241</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Okumura, Teppei</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Kayo, Issha</style></author><author><style face="normal" font="default" size="100%">Hikage, Chiaki</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...676..889O</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">676</style></volume><pages><style face="normal" font="default" size="100%">889-898</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We study the large-scale anisotropic two-point correlation functionusing 46,760 luminous red galaxies at redshifts 0.16-0.47 from the SloanDigital Sky Survey. We measure the correlation function as a function ofseparations parallel and perpendicular to the line of sight in order totake account of anisotropy of the large-scale structure in redshiftspace. We find a slight signal of baryonic features in the anisotropiccorrelation function, i.e., a ``baryon ridge'' corresponding to a baryonacoustic peak in the spherically averaged correlation function, whichhas already been reported using the same sample. The baryon ridge hasprimarily a spherical structure with a known radius in comovingcoordinates. It enables us to divide the redshift distortion effectsinto dynamical and geometrical components and provides furtherconstraints on cosmological parameters, including the dark energyequation-of-state. With an assumption of a flat Λ cosmology, wefind the best-fit values ofΩ&lt;sub&gt;m&lt;/sub&gt;=0.218&lt;sup&gt;+0.047&lt;/sup&gt;&lt;sub&gt;-0.037&lt;/sub&gt; and&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0711.3640</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Assef, R. J.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Brodwin, M.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, A. H.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Jones, C.</style></author><author><style face="normal" font="default" size="100%">McKenzie, E.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Low-Resolution Spectral Templates for Galaxies from 0.2 to 10 μm</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...676..286A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">676</style></volume><pages><style face="normal" font="default" size="100%">286-303</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We built an optimal basis of low-resolution templates for galaxies overthe wavelength range from 0.2 to 10 μm using a variant of thealgorithm presented by Budavari and coworkers. We derived them using 11bands of photometry from the NDWFS, FLAMEX, zBoötes, and IRACShallow surveys for 16,033 galaxies in the NDWFS Boötes field withspectroscopic redshifts measured by the AGN and Galaxy Evolution Survey.We also developed algorithms to accurately determine photometricredshifts, K-corrections, and bolometric luminosities using thesetemplates. Our photometric redshifts have an accuracy of&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0708.1513</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Jiang, Linhua</style></author><author><style face="normal" font="default" size="100%">Maraston, Claudia</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Luminosity Function Constraints on the Evolution of Massive Red Galaxies since z ~ 0.9</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...682..919C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">682</style></volume><pages><style face="normal" font="default" size="100%">919-936</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We measure the evolution of the luminous red galaxy (LRG) luminosityfunction in the redshift range 0.12, minimizing the impact oflarge-scale structure on our results. We find that the LRG populationhas evolved little beyond the passive fading of its stellar populationssince z~0.9. Based on our luminosity function measurements and assuminga nonevolving Salpeter stellar initial mass function, we find that themost massive (L&amp;gt;3L&lt;sup&gt;*&lt;/sup&gt;) red galaxies have grown by less than&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0804.4516</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, Rodger I.</style></author><author><style face="normal" font="default" size="100%">Bechtold, Jill</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Arnett, David</style></author><author><style face="normal" font="default" size="100%">Martins, Carlos</style></author><author><style face="normal" font="default" size="100%">Kennicutt, Robert</style></author><author><style face="normal" font="default" size="100%">Black, John</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A molecular probe of dark energy</style></title><secondary-title><style face="normal" font="default" size="100%">Advances in Space Research</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008AdSpR..42..596T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">42</style></volume><pages><style face="normal" font="default" size="100%">596-598</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Many theoretical models of dark energy invoke rolling scaler fieldswhich in turn predict time varying values of the fundamental constants.Establishing the value of the fundamental constants at various times inthe universe can probe and test the various dark energy theories. One ofthe constants that is predicted to vary is the ratio of the electron toproton mass μ. It was established early on that molecular spectra aresensitive to the value of μ and can be used as probes of that value.This article describes the use of the spectrum of molecular hydrogen inhigh redshift Damped Lyman Alpha systems (DLAs) as a sensitive probe ofthe time evolution of μ.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1016/j.asr.2007.07.009</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Siegel, Ethan R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Nonlinear Structure Formation and the Acoustic Scale</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...686...13S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">686</style></volume><pages><style face="normal" font="default" size="100%">13-24</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present high signal-to-noise ratio measurements of the acoustic scalein the presence of nonlinear growth and redshift distortions using 320h&lt;sup&gt;-3&lt;/sup&gt; Gpc&lt;sup&gt;3&lt;/sup&gt; of cosmological particle-meshsimulations. Using simple fitting methods, we obtain robust measurementsof the acoustic scale with scatter close to that predicted by the Fishermatrix. We detect and quantify the shift in the acoustic scale byanalyzing the power spectrum: we detect at greater than 5 σ adecrease in the acoustic scale in the real-space matter power spectrum&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0805.0117</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Observing dark energy</style></title><secondary-title><style face="normal" font="default" size="100%">Classical and Quantum Gravity</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008CQGra..25k4001E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">25</style></volume><pages><style face="normal" font="default" size="100%">4001</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;I review the observational evidence for dark energy, arguing that thelarge-scale structure observed at low redshift and in the cosmicmicrowave background offers a strong corroboration of the supernova Iaresults. The angular scale of the acoustic oscillations in the cosmicmicrowave background strongly support a nearly flat universe, while manyarguments from low-redshift cosmology support a matter density around&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1088/0264-9381/25/11/114001</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Passive Evolution of Galaxy Clustering</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...681..998S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">681</style></volume><pages><style face="normal" font="default" size="100%">998-1016</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a numerical study of the evolution of galaxy clustering whengalaxies flow passively from high redshift, respecting the continuityequation throughout. While passive flow is a special case of galaxyevolution, it allows a well-defined study of galaxy ancestry and servesas an interesting limit to be compared to nonpassive cases. We usedissipationless N-body simulations, assign galaxies to massive halos atz=1 and 2 using various halo occupation distribution (HOD) models, andtrace these galaxy particles to lower redshift while conserving theirnumber. We find that passive flow results in an asymptotic convergenceat low redshift in the HOD and in galaxy clustering on scales above ~3h&lt;sup&gt;-1&lt;/sup&gt; Mpc for a wide range of initial HODs. As galaxies becomeless biased with respect to mass asymptotically with time, the HODparameters evolve such that M&lt;sub&gt;1&lt;/sub&gt;/M&lt;sub&gt;min&lt;/sub&gt; decreaseswhile α converges toward unity, whereg(M)&amp;gt;=exp(-M&lt;sub&gt;min&lt;/sub&gt;/M)[1+(M/M&lt;sub&gt;1&lt;/sub&gt;)&lt;sup&gt;α&lt;/sup&gt;].The satellite populations converge toward the Poisson distribution atlow redshift. The convergence is robust for different number densitiesand is enhanced when galaxies evolve from higher redshift. We compareour results with the observed luminous red galaxy (LRG) sample from SDSSthat has the same number density. We claim that if LRGs have experienceda strict passive flow, their g(M)&amp;gt; should be close toa power law with an index of unity in halo mass. Discrepancies could bedue to dry galaxy merging or new members arising between the initial andthe final redshifts. The spatial distribution of passively flowinggalaxies within halos appears on average more concentrated than the halomass profile at low redshift. The evolution of bias for passivelyflowing galaxies is consistent with linear bias evolution onquasi-linear as well as large scales.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0712.1643</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Anderson, Kurt S. J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bailer-Jones, C. A. L.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Bassett, Bruce A.</style></author><author><style face="normal" font="default" size="100%">Becker, Andrew C.</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Bell, Eric F.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brinchmann, Jarle</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carliles, Samuel</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Cinabro, David</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Covey, Kevin R.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Cunha, Carlos E.</style></author><author><style face="normal" font="default" size="100%">Davenport, James R. A.</style></author><author><style face="normal" font="default" size="100%">Dilday, Ben</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gänsicke, Boris T.</style></author><author><style face="normal" font="default" size="100%">Gates, Evalyn</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Gurbani, Vijay K.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Harding, Paul</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hayes, Jeffrey</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hirata, Christopher M.</style></author><author><style face="normal" font="default" size="100%">Hogan, Craig J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Hyde, Joseph B.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnson, Jennifer A.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kessler, R.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Kuropatkin, Nikolay</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lebedeva, Svetlana</style></author><author><style face="normal" font="default" size="100%">Lee, Young Sun</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Lépine, Sébastien</style></author><author><style face="normal" font="default" size="100%">Lima, Marcos</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loomis, Craig P.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Olena</style></author><author><style face="normal" font="default" size="100%">Malanushenko, Viktor</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Marriner, John P.</style></author><author><style face="normal" font="default" size="100%">Martínez-Delgado, David</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Morrison, Heather L.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Oyaizu, Hiroaki</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Park, Changbom</style></author><author><style face="normal" font="default" size="100%">Peoples, John, Jr.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Purger, Norbert</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Re Fiorentin, Paola</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Riess, Adam G.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Sako, Masao</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schreiber, Matthias R.</style></author><author><style face="normal" font="default" size="100%">Schwope, Axel D.</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sesar, Branimir</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Sivarani, Thirupathi</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Steinmetz, Matthias</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Suto, Yasushi</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vidrih, S.</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Wadadekar, Yogesh</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilhite, Brian C.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sixth Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJS..175..297A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">175</style></volume><pages><style face="normal" font="default" size="100%">297-313</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper describes the Sixth Data Release of the Sloan Digital SkySurvey. With this data release, the imaging of the northern Galactic capis now complete. The survey contains images and parameters of roughly287 million objects over 9583 deg&lt;sup&gt;2&lt;/sup&gt;, including scans over alarge range of Galactic latitudes and longitudes. The survey alsoincludes 1.27 million spectra of stars, galaxies, quasars, and blank sky(for sky subtraction) selected over 7425 deg&lt;sup&gt;2 &lt;/sup&gt;. This releaseincludes much more stellar spectroscopy than was available in previousdata releases and also includes detailed estimates of stellartemperatures, gravities, and metallicities. The results of improvedphotometric calibration are now available, with uncertainties of roughly&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0707.3413</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Shin, Min-Su</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">White, Richard L.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Kayo, Issha</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Clocchiatti, Alejandro</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Kawano, Yozo</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Morokuma, Tomoki</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin Scott</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Masataka, Fukugita</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey Quasar Lens Search. II. Statistical Lens Sample from the Third Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008AJ....135..496I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">135</style></volume><pages><style face="normal" font="default" size="100%">496-511</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the first results of our systematic search for strongly lensedquasars using the spectroscopically confirmed quasars in the SloanDigital Sky Survey (SDSS). Among 46,420 quasars from the SDSS DataRelease 3 (~4188 deg&lt;sup&gt;2&lt;/sup&gt;), we select a subsample of 22,683quasars that are located at redshifts between 0.6 and 2.2 and arebrighter than the Galactic extinction-corrected i-band magnitude of19.1. We identify 220 lens candidates from the quasar subsample, forwhich we conduct extensive and systematic follow-up observations inoptical and near-infrared wavebands, in order to construct a completelensed quasar sample at image separations between 1'' and 20'' and fluxratios of faint to bright lensed images larger than 10&lt;sup&gt;-0.5&lt;/sup&gt;.We construct a statistical sample of 11 lensed quasars. Ten of these aregalaxy-scale lenses with small image separations (~ 1''-2'') and one isa large separation (15'') system which is produced by a massive clusterof galaxies, representing the first statistical sample of lensed quasarsincluding both galaxy- and cluster-scale lenses. The Data Release 3spectroscopic quasars contain an additional 11 lensed quasars outsidethe statistical sample.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0708.0828</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Kayo, Issha</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Shin, Min-Su</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">White, Richard L.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Clocchiatti, Alejandro</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Kawano, Yozo</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert</style></author><author><style face="normal" font="default" size="100%">Morokuma, Tomoki</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin Scott</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey Quasar Lens Search. III. Constraints on Dark Energy from the Third Data Release Quasar Lens Catalog</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008AJ....135..512O</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">135</style></volume><pages><style face="normal" font="default" size="100%">512-519</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present cosmological results from the statistics of lensed quasars inthe Sloan Digital Sky Survey (SDSS) Quasar Lens Search. By taking properaccount of the selection function, we compute the expected number ofquasars lensed by early-type galaxies and their image separationdistribution assuming a flat universe, which is then compared with sevenlenses found in the SDSS Data Release 3 to derive constraints on darkenergy under strictly controlled criteria. For a cosmological constantmodel (w = -1) we obtain Ω&lt;sub&gt;Λ&lt;/sub&gt; =0.74&lt;sup&gt;+0.11&lt;/sup&gt; &lt;sub&gt;-0.15&lt;/sub&gt;(stat.)&lt;sup&gt;+0.13&lt;/sup&gt;&lt;sub&gt;-0.06&lt;/sub&gt;(syst.). Allowing w to be a free parameter we findΩ&lt;sub&gt;M&lt;/sub&gt; = 0.26&lt;sup&gt;+0.07&lt;/sup&gt;&lt;sub&gt;-0.06&lt;/sub&gt;(stat.)&lt;sup&gt;+0.03&lt;/sup&gt; &lt;sub&gt;-0.05&lt;/sub&gt;(syst.) and w =-1.1 ± 0.6(stat.)&lt;sup&gt;+0.3&lt;/sup&gt; &lt;sub&gt;-0.5&lt;/sub&gt;(syst.) whencombined with the constraint from the measurement of baryon acousticoscillations in the SDSS luminous red galaxy sample. Our results are ingood agreement with earlier lensing constraints obtained using radiolenses, and provide additional confirmation of the presence of darkenergy consistent with a cosmological constant, derived independently oftype Ia supernovae.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0708.0825</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Stutz, Amelia M.</style></author><author><style face="normal" font="default" size="100%">Papovich, Casey</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">On the Stellar Populations in Faint Red Galaxies in the Hubble Ultra Deep Field</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2008</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2008</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2008ApJ...677..828S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">677</style></volume><pages><style face="normal" font="default" size="100%">828-845</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We study the nature of faint red-selected galaxies at z~2-3 using theHubble Ultra Deep Field (HUDF) and Spitzer Infrared Array Camera (IRAC)photometry. Given the magnitude limit of the HST data, we detectcandidate galaxies to H&lt;sub&gt;AB&lt;/sub&gt;&amp;lt;26 mag, probing lower luminosity(lower mass) galaxies at these redshifts. We identify 32 galaxiessatisfying the (J&lt;sub&gt;110&lt;/sub&gt;-H&lt;sub&gt;160&lt;/sub&gt;)&lt;sub&gt;AB&lt;/sub&gt;&amp;gt;1.0 magcolor selection, 16 of which have unblended [3.6 μm] and [4.5 μm]photometry from Spitzer. Using this multiwavelength data set, we derivephotometric redshifts, masses, and stellar population parameters forthese objects. We find that the selected objects span a diverse range ofproperties over a large range of redshifts, 1&amp;lt;~z&amp;lt;~3.5. Asubstantial fraction (11/32) of the(J&lt;sub&gt;110&lt;/sub&gt;-H&lt;sub&gt;160&lt;/sub&gt;)&lt;sub&gt;AB&lt;/sub&gt;&amp;gt;1.0 mag populationappear to be lower redshift (z&amp;lt;~2.5), heavily obscured dusty galaxiesor edge-on spiral galaxies, while others (12/32) appear to be galaxiesat 2&amp;lt;~z&amp;lt;~3.5 whose light at rest-frame optical wavelengths isdominated by evolved stellar populations. We argue that longerwavelength data (&amp;gt;~1 μm, rest frame) are essential forinterpreting the properties of the stellar populations in red-selectedgalaxies at these redshifts. Interestingly, by including Spitzer data,many candidates for galaxies dominated by evolved stellar populationsare rejected, and for only a subset of the sample (6/16) do the datafavor this interpretation. These objects have a surface density of ~1arcmin&lt;sup&gt;-2&lt;/sup&gt;. We place an upper limit on the space density ofcandidate massive evolved galaxies with 2.5AB160&amp;lt;=26 mag ofn=6.6&lt;sup&gt;+2.0&lt;/sup&gt;&lt;sub&gt;-3.0&lt;/sub&gt;×10&lt;sup&gt;-4&lt;/sup&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;, with a corresponding upper limit on the stellar massdensity ofρ&lt;sup&gt;*&lt;/sup&gt;=5.6&lt;sup&gt;+4.4&lt;/sup&gt;&lt;sub&gt;-2.8&lt;/sub&gt;×10&lt;sup&gt;7&lt;/sup&gt;M&lt;sub&gt;solar&lt;/sub&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. The z&amp;gt;2.5 objects that aredominated by evolved stellar populations have a space density at mostone-third that of z~0 red early-type galaxies. Therefore, at leasttwo-thirds of present-day early-type galaxies assemble or evolve intotheir current configuration at redshifts below 2.5. We find a dearth ofcandidates for low-mass (&amp;lt;~2×10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;solar&lt;/sub&gt;)galaxies at 1.5&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0801.2388</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">da Ângela, J.</style></author><author><style face="normal" font="default" size="100%">Shanks, T.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Cannon, Russell D.</style></author><author><style face="normal" font="default" size="100%">Edge, A. C.</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Outram, P. J.</style></author><author><style face="normal" font="default" size="100%">Colless, Matthew</style></author><author><style face="normal" font="default" size="100%">Couch, Warrick J.</style></author><author><style face="normal" font="default" size="100%">Croom, Scott M.</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin A.</style></author><author><style face="normal" font="default" size="100%">Roseboom, Isaac G.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Sharp, Robert G.</style></author><author><style face="normal" font="default" size="100%">Weilbacher, P. M.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The 2dF-SDSS LRG and QSO Survey: the LRG 2-point correlation function and redshift-space distortions</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.381..573R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">381</style></volume><pages><style face="normal" font="default" size="100%">573-588</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a clustering analysis of luminous red galaxies (LRGs) usingnearly 9000 objects from the final, three-year catalogue of the 2dF-SDSSLRG and QSO (2SLAQ) Survey. We measure the redshift-space two-pointcorrelation function, ξ(s) and find that, at the mean LRG redshift ofshows the characteristic downturn at small scales(&amp;lt;~1h&lt;sup&gt;-1&lt;/sup&gt;Mpc) expected from line-of-sight velocitydispersion. We fit a double power law to ξ(s) and measure anamplitude and slope of s&lt;sub&gt;0&lt;/sub&gt; =17.3&lt;sup&gt;+2.5&lt;/sup&gt;&lt;sub&gt;-2.0&lt;/sub&gt;h&lt;sup&gt;-1&lt;/sup&gt;Mpc,γ = 1.03 +/-0.07 at small scales (s &amp;lt; 4.5h&lt;sup&gt;-1&lt;/sup&gt;Mpc) and s&lt;sub&gt;0&lt;/sub&gt; =9.40 +/- 0.19h&lt;sup&gt;-1&lt;/sup&gt;Mpc,γ = 2.02 +/- 0.07 at large scales(s &amp;gt; 4.5h&lt;sup&gt;-1&lt;/sup&gt;Mpc). In the semiprojected correlationfunction, w&lt;sub&gt;p&lt;/sub&gt;(σ), we find a simple power law withγ = 1.83 +/- 0.05 and r&lt;sub&gt;0&lt;/sub&gt; = 7.30 +/-0.34h&lt;sup&gt;-1&lt;/sup&gt;Mpc fits the data in the range 0.4 &amp;lt; σ &amp;lt;50h&lt;sup&gt;-1&lt;/sup&gt;Mpc, although there is evidence of a steeper power lawat smaller scales. A single power law also fits the deprojectedcorrelation function ξ(r), with a correlation length of r&lt;sub&gt;0&lt;/sub&gt;= 7.45 +/- 0.35h&lt;sup&gt;-1&lt;/sup&gt;Mpc and a power-law slope of γ = 1.72+/- 0.06 in the 0.4 &amp;lt; r &amp;lt; 50h&lt;sup&gt;-1&lt;/sup&gt;Mpc range. But it is inthe LRG angular correlation function that the strongest evidence fornon-power-law features is found where a slope of γ = -2.17 +/-0.07 is seen at 1 &amp;lt; r &amp;lt; 10h&lt;sup&gt;-1&lt;/sup&gt;Mpc with a flatter γ= -1.67 +/- 0.07 slope apparent at r &amp;lt;~ 1h&lt;sup&gt;-1&lt;/sup&gt;Mpc scales.We use the simple power-law fit to the galaxy ξ(r), under theassumption of linear bias, to model the redshift-space distortions inthe 2D redshift-space correlation function, ξ(σ, π). We fitfor the LRG velocity dispersion, w&lt;sub&gt;z&lt;/sub&gt;, the density parameter,Ω&lt;sub&gt;m&lt;/sub&gt; and β(z), where β(z) =Ω&lt;sup&gt;0.6&lt;/sup&gt;&lt;sub&gt;m&lt;/sub&gt;/b and b is the linear bias parameter.We find values of w&lt;sub&gt;z&lt;/sub&gt; =330kms&lt;sup&gt;-1&lt;/sup&gt;,Ω&lt;sub&gt;m&lt;/sub&gt; =0.10&lt;sup&gt;+0.35&lt;/sup&gt;&lt;sub&gt;-0.10&lt;/sub&gt; and β = 0.40 +/- 0.05. The lowvalues for w&lt;sub&gt;z&lt;/sub&gt; and β reflect the high bias of the LRGsample. These high-redshift results, which incorporate theAlcock-Paczynski effect and the effects of dynamical infall, start tobreak the degeneracy between Ω&lt;sub&gt;m&lt;/sub&gt; and β found inlow-redshift galaxy surveys such as 2dFGRS. This degeneracy is furtherbroken by introducing an additional external constraint, which is thevalue β(z = 0.1) = 0.45 from 2dFGRS, and then considering theevolution of clustering from z ~ 0 to z&lt;sub&gt;LRG&lt;/sub&gt; ~ 0.55. With thesecombined methods we find Ω&lt;sub&gt;m&lt;/sub&gt;(z = 0) = 0.30 +/- 0.15 andβ(z = 0.55) = 0.45 +/- 0.05. Assuming these values, we find a valuefor b(z = 0.55) = 1.66 +/- 0.35. We show that this is consistent with asimple `high-peak' bias prescription which assumes that LRGs have aconstant comoving density and their clustering evolves purely undergravity.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0612400</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Makarov, Alexey</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jonathan</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The clustering of luminous red galaxies in the Sloan Digital Sky Survey imaging data</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.378..852P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">378</style></volume><pages><style face="normal" font="default" size="100%">852-872</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the 3D real-space clustering power spectrum of a sample of~600000 luminous red galaxies measured by the Sloan Digital Sky Survey,using photometric redshifts. These galaxies are old, elliptical systemswith strong 4000-Å breaks, and have accurate photometric redshiftswith an average error of Δz = 0.03. This sample of galaxies rangesfrom redshift z = 0.2 to 0.6 over 3528 deg&lt;sup&gt;2&lt;/sup&gt; of the sky,probing a volume of 1.5h&lt;sup&gt;-3&lt;/sup&gt;Gpc&lt;sup&gt;3&lt;/sup&gt;, making it thelargest volume ever used for galaxy clustering measurements. We measurethe angular clustering power spectrum in eight redshift slices and usewell-calibrated redshift distributions to combine these into ahigh-precision 3D real-space power spectrum from k = 0.005 to k =1hMpc&lt;sup&gt;-1&lt;/sup&gt;. We detect power on gigaparsec scales, beyond theturnover in the matter power spectrum, at a ~2σ significance for k&amp;lt; 0.01hMpc&lt;sup&gt;-1&lt;/sup&gt;, increasing to 5.5σ for k &amp;lt;0.02hMpc&lt;sup&gt;-1&lt;/sup&gt;. This detection of power is on scalessignificantly larger than those accessible to current spectroscopicredshift surveys. We also find evidence for baryonic oscillations, bothin the power spectrum, as well as in fits to the baryon density, at a2.5 σ confidence level. The large volume and resulting smallstatistical errors on the power spectrum allow us to constrain both theamplitude and the scale dependence of the galaxy bias in cosmologicalfits. The statistical power of these data to constrain cosmology is ~1.7times better than previous clustering analyses. Varying the matterdensity and baryon fraction, we find Ω&lt;sub&gt;M&lt;/sub&gt; = 0.30 +/-0.03, and Ω&lt;sub&gt;b&lt;/sub&gt;/Ω&lt;sub&gt;M&lt;/sub&gt; = 0.18 +/- 0.04, for afixed Hubble constant of 70kms&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-1&lt;/sup&gt; and ascale-invariant spectrum of initial perturbations. The detection ofbaryonic oscillations also allows us to measure the comoving distance toz = 0.5; we find a best-fitting distance of 1.73 +/- 0.12Gpc,corresponding to a 6.5 per cent error on the distance. These resultsdemonstrate the ability to make precise clustering measurements withphotometric surveys.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0605302</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, Rodger I.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia</style></author><author><style face="normal" font="default" size="100%">Kennicutt, Robert C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Constraints on the Cosmic Near-Infrared Background Excess from NICMOS Deep Field Observations</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...657..669T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">657</style></volume><pages><style face="normal" font="default" size="100%">669-680</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;NICMOS observations of the resolved object fluxes in the Hubble DeepField-North and the Hubble Ultra Deep Field are significantly below thefluxes attributed to a 1.4-1.8 μm near-infrared background excess(NIRBE) from previous low spatial resolution NIRS measurements. Testsplacing sources in the NICMOS image with fluxes sufficient to accountfor the NIRBE indicate that the NIRBE flux must be either flat on scalesgreater than 100&quot; or clumped on scales of several arcminutes to avoiddetection in the NICMOS image. A fluctuation analysis of the new NICMOSdata shows a fluctuation spectrum consistent with that found at the samewavelength in deep 2MASS calibration images. The fluctuation analysisshows that the majority of the fluctuation power comes from resolvedgalaxies at redshifts of 1.5 and less and that the fluctuations observedin the earlier deep 2MASS observations can be completely accounted forwith normal low-redshift galaxies. Neither the NICMOS direct fluxmeasurements nor the fluctuation analysis require an additionalcomponent of near-infrared flux other than the flux from normal resolvedgalaxies in the redshift range between 0 and 7. The residualfluctuations in the angular range between 1&quot; and 10&quot; is 1-2 nWm&lt;sup&gt;-2&lt;/sup&gt; sr&lt;sup&gt;-1&lt;/sup&gt;, which is at or above several predictionsof fluctuations from high redshift Population III objects, butinconsistent with attributing the entire NIRBE to high-redshiftgalaxies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0612033</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">McDonald, Patrick</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Dark energy and curvature from a future baryonic acoustic oscillation survey using the Lyman-α forest</style></title><secondary-title><style face="normal" font="default" size="100%">Physical Review D</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007PhRvD..76f3009M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">76</style></volume><pages><style face="normal" font="default" size="100%">63009</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We explore the requirements for a Lyman-α forest survey designedto measure the angular diameter distance and Hubble parameter at2≲z≲4 using the standard ruler provided by baryonic acousticoscillations (BAO). The goal would be to obtain a high enough density ofsources to probe the three-dimensional density field on the scale of theBAO feature. A percent-level measurement in this redshift range canalmost double the Dark Energy Task Force figure of merit, relative tothe case with only a similar precision measurement at z˜1, if theUniverse is not assumed to be flat. This improvement is greater than theone obtained by doubling the size of the z˜1 survey, with Planckand a weak Sloan Digital Sky Survey-like z=0.3 BAO measurement assumedin each case. Galaxy BAO surveys at z˜1 may be able to make aneffective Lyα forest measurement simultaneously at minimal addedcost, because the required number density of quasars is relativelysmall. We discuss the constraining power as a function of area,magnitude limit (density of quasars), resolution, and signal-to-noise ofthe spectra. For example, a survey covering 2000 sq. deg. and achievingS/N=1.8 per Å at g=23 (˜40quasars per sq. deg.) with anR≳250 spectrograph is sufficient to measure both the radial and&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0607122</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Borra, Ermanno F.</style></author><author><style face="normal" font="default" size="100%">Seddiki, Omar</style></author><author><style face="normal" font="default" size="100%">Angel, Roger</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hickson, Paul</style></author><author><style face="normal" font="default" size="100%">Seddon, Kenneth R.</style></author><author><style face="normal" font="default" size="100%">Worden, Simon P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Deposition of metal films on an ionic liquid as a basis for a lunar telescope</style></title><secondary-title><style face="normal" font="default" size="100%">Nature</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007Natur.447..979B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">447</style></volume><pages><style face="normal" font="default" size="100%">979-981</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;An optical/infrared telescope of 20-100m aperture located on the Moonwould be able to observe objects 100 to 1,000 times fainter than theproposed next generation of space telescopes. The infrared region of thespectrum is particularly important for observations of objects atredshifts z&amp;gt;7. The apparent simplicity and low mass of a liquidmirror telescope, compared with a traditional pointable glass mirror,suggest that the concept should be considered further. A previouslyproposed liquid mirror telescope, based upon a spinning liquid metallicalloy, is not appropriate for infrared applications, which will requirea liquid below 130K. Here we report the successful coating of an ionicliquid with silver. The surface is smooth and the silver coating isstable on a timescale of months. The underlying ionic liquid does notevaporate in a vacuum and remains liquid down to a temperature of 175K.Given that there are ~10&lt;sup&gt;6&lt;/sup&gt; simple and ~10&lt;sup&gt;18&lt;/sup&gt; ternaryionic liquids, it should be possible to synthesize liquids with evenlower melting temperatures.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1038/nature05909</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, Rodger I.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia</style></author><author><style face="normal" font="default" size="100%">Kennicutt, Robert C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Evidence for a z &lt; 8 Origin of the Source-subtracted Near-Infrared Background</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...666..658T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">666</style></volume><pages><style face="normal" font="default" size="100%">658-662</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper extends our previous fluctuation analysis of thenear-infrared background at 1.6 μm to the 1.1 μm (F110W) image ofthe Hubble Ultra Deep Field. When all detectable sources are removed,the ratio of fluctuation power in the two images is consistent with theratio expected for faint, z&amp;lt;8, sources, and is inconsistent with theexpected ratio for galaxies with z&amp;gt;8. We also use numericallyredshifted model galaxy spectral energy distributions for 50 and 10 Myrold galaxies to predict the expected fluctuation power at 3.6 and 4.5μm to compare with recent Spitzer observations. The predictedfluctuation power for galaxies at z=0-12 matches the observed  Spitzerfluctuation power, while the predicted power for z&amp;gt;13 galaxies ismuch higher than the observed values. As was found in the 1.6 μm(F160W) analysis, the fluctuation power in the source-subtracted F110Wimage is 2 orders of magnitude below the power in the image with allsources present. This leads to the conclusion that the 0.8-1.8 μmnear-infrared background is due to resolved galaxies in the redshiftrange z&amp;lt;8, with the majority of power in the redshift range of0.5-1.5.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0706.0547</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Anderson, Kurt S. J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bailer-Jones, Coryn A. L.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Belokurov, V.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Bramich, D. M.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinchmann, Jarle</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carey, Larry N.</style></author><author><style face="normal" font="default" size="100%">Carliles, Samuel</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Cunha, Carlos E.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Dalcanton, Julianne J.</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Evans, N. W.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Gilmore, G.</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">de Haas, Ernst</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hayes, Jeffrey</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hirata, Christopher M.</style></author><author><style face="normal" font="default" size="100%">Hogan, Craig J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Takashi</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kauffmann, Guinevere</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kniazev, Alexei Yu.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Kuropatkin, Nikolay</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Lima, Marcos</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Martínez-Delgado, David</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Nash, Thomas</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Oyaizu, Hiroaki</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Park, Changbom</style></author><author><style face="normal" font="default" size="100%">Peoples, John, Jr.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Pourbaix, Dimitri</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas R.</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Re Fiorentin, Paola</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Suto, Yasushi</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vidrih, S.</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilhite, Brian</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zibetti, Stefano</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Fifth Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJS..172..634A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">172</style></volume><pages><style face="normal" font="default" size="100%">634-644</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper describes the Fifth Data Release (DR5) of the Sloan DigitalSky Survey (SDSS). DR5 includes all survey quality data taken through2005 June and represents the completion of the SDSS-I project (whosesuccessor, SDSS-II, will continue through mid-2008). It includesfive-band photometric data for 217 million objects selected over 8000deg&lt;sup&gt;2&lt;/sup&gt; and 1,048,960 spectra of galaxies, quasars, and starsselected from 5713 deg&lt;sup&gt;2&lt;/sup&gt; of that imaging data. These numbers&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0707.3380</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Improved Forecasts for the Baryon Acoustic Oscillations and Cosmological Distance Scale</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...665...14S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">665</style></volume><pages><style face="normal" font="default" size="100%">14-24</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the cosmological distance errors achievable using thebaryonic acoustic oscillations as a standard ruler. We begin from aFisher matrix formalism that is upgraded from earlier Seo and Eisensteinwork. We isolate the information from the baryonic peaks by excludingdistance information from other less robust sources. Meanwhile, weaccommodate the Lagrangian displacement distribution into the Fishermatrix calculation to reflect the gradual loss of information in scaleand in time due to nonlinear growth, nonlinear bias, and nonlinearredshift distortions. We then show that we can contract themultidimensional Fisher matrix calculations into a two-dimensional oreven one-dimensional formalism with physically motivated approximations.We present the resulting fitting formula for the cosmological distanceerrors from galaxy redshift surveys as a function of survey parametersand nonlinearity, which saves us going through the 12 dimensional Fishermatrix calculations. Finally, we show excellent agreement between thedistance error estimates from the revised Fisher matrix and theprecision on the distance scale recovered from N-body simulations.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0701079</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Sirko, Edwin</style></author><author><style face="normal" font="default" size="100%">Spergel, David N.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Improving Cosmological Distance Measurements by Reconstruction of the Baryon Acoustic Peak</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...664..675E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">664</style></volume><pages><style face="normal" font="default" size="100%">675-679</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The baryon acoustic oscillations are a promising route to the precisionmeasure of the cosmological distance scale and hence the measurement ofthe time evolution of dark energy. We show that the nonlineardegradation of the acoustic signature in the correlations oflow-redshift galaxies is a correctable process. By suitablereconstruction of the linear density field, one can sharpen the acousticpeak in the correlation function or, equivalently, restore the higherharmonics of the oscillations in the power spectrum. With this, one canachieve better measurements of the acoustic scale for a given surveyvolume. Reconstruction is particularly effective at low redshift, wherethe nonlinearities are worse but where the dark energy density ishighest. At z=0.3, we find that one can reduce the sample variance errorbar on the acoustic scale by at least a factor of 2 and in principle bynearly a factor of 4. We discuss the significant implications ourresults have for the design of galaxy surveys aimed at measuring thedistance scale through the acoustic peak.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0604362</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hickox, R. C.</style></author><author><style face="normal" font="default" size="100%">Jones, C.</style></author><author><style face="normal" font="default" size="100%">Forman, W. R.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Brodwin, M.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P. R.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Dey, A.</style></author><author><style face="normal" font="default" size="100%">Brand, K.</style></author><author><style face="normal" font="default" size="100%">Gorjian, V.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Large Population of Mid-Infrared-selected, Obscured Active Galaxies in the Boötes Field</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...671.1365H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">671</style></volume><pages><style face="normal" font="default" size="100%">1365-1387</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We identify a population of 640 obscured and 839 unobscured AGNs atredshifts 0.72 NOAO Deep Wide-Field Survey (NDWFS) region inBoötes. We select AGNs on the basis of Spitzer IRAC colors obtainedby the IRAC Shallow Survey. Redshifts are obtained from opticalspectroscopy or photometric redshift estimators. We classify theIR-selected AGNs as IRAGN 1 (unobscured) and IRAGN 2 (obscured) using asimple criterion based on the observed optical to mid-IR color, with aselection boundary of R-[4.5]=6.1, where R and [4.5] are the Vegamagnitudes in the  R and IRAC 4.5 μm bands, respectively. We verifythis selection using X-ray stacking analyses with data from the ChandraXBoötes survey, as well as optical photometry from NDWFS andspectroscopy from MMT/AGES. We show that (1) these sources are indeedAGNs, and (2) the optical/IR color selection separates obscured sources(with average N&lt;sub&gt;H&lt;/sub&gt;~3×10&lt;sup&gt;22&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;obtained from X-ray hardness ratios, and optical colors and morphologiestypical of galaxies) and unobscured sources (with no X-ray absorption,&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0708.3678</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Huang, J.-S.</style></author><author><style face="normal" font="default" size="100%">Ashby, M. L. N.</style></author><author><style face="normal" font="default" size="100%">Barmby, P.</style></author><author><style face="normal" font="default" size="100%">Brodwin, M.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Cool, R. J.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Fazio, G. G.</style></author><author><style face="normal" font="default" size="100%">Le Floc'h, E.</style></author><author><style face="normal" font="default" size="100%">Green, P.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">Lu, Nanyao</style></author><author><style face="normal" font="default" size="100%">Pahre, M. A.</style></author><author><style face="normal" font="default" size="100%">Rigopoulou, D.</style></author><author><style face="normal" font="default" size="100%">Rosenberg, J. L.</style></author><author><style face="normal" font="default" size="100%">Smith, H. A.</style></author><author><style face="normal" font="default" size="100%">Wang, Z.</style></author><author><style face="normal" font="default" size="100%">Willmer, C. N. A.</style></author><author><style face="normal" font="default" size="100%">Willner, S. P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Local Galaxy 8 μm Luminosity Function</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...664..840H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">664</style></volume><pages><style face="normal" font="default" size="100%">840-849</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;A Spitzer Space Telescope survey in the NOAO Deep Wide Field inBoötes provides a complete, 8 μm-selected sample of galaxies toa limiting (Vega) magnitude of 13.5. In the 6.88 deg&lt;sup&gt;2&lt;/sup&gt; field&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0704.3609</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Cole, Shaun</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Peacock, John A.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Measuring the Baryon Acoustic Oscillation scale using the Sloan Digital Sky Survey and 2dF Galaxy Redshift Survey</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.381.1053P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">381</style></volume><pages><style face="normal" font="default" size="100%">1053-1066</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We introduce a method to constrain general cosmological models usingBaryon Acoustic Oscillation (BAO) distance measurements from galaxysamples covering different redshift ranges, and apply this method toanalyse samples drawn from the Sloan Digital Sky Survey (SDSS) and 2dFGalaxy Redshift Survey (2dFGRS). BAOs are detected in the clustering ofthe combined 2dFGRS and SDSS main galaxy samples, and measure thedistance-redshift relation at z = 0.2. BAOs in the clustering of theSDSS luminous red galaxies measure the distance-redshift relation at z =0.35. The observed scales of the BAOs calculated from these samples andfrom the combined sample are jointly analysed using estimates of thecorrelated errors, to constrain the form of the distance measureD&lt;sub&gt;V&lt;/sub&gt;(z) ≡ [(1 +z)&lt;sup&gt;2&lt;/sup&gt;D&lt;sup&gt;2&lt;/sup&gt;&lt;sub&gt;A&lt;/sub&gt;cz/H(z)]&lt;sup&gt;1/3&lt;/sup&gt;. HereD&lt;sub&gt;A&lt;/sub&gt; is the angular diameter distance, and H(z) is the Hubbleparameter. This gives r&lt;sub&gt;s&lt;/sub&gt;/D&lt;sub&gt;V&lt;/sub&gt;(0.2) = 0.1980 +/-0.0058 and r&lt;sub&gt;s&lt;/sub&gt;/D&lt;sub&gt;V&lt;/sub&gt;(0.35) = 0.1094 +/- 0.0033(1σ errors), with a correlation coefficient of 0.39, wherer&lt;sub&gt;s&lt;/sub&gt; is the comoving sound horizon scale at recombination.Matching the BAOs to have the same measured scale at all redshifts thengives D&lt;sub&gt;V&lt;/sub&gt;(0.35)/D&lt;sub&gt;V&lt;/sub&gt;(0.2) = 1.812 +/- 0.060. Therecovered ratio is roughly consistent with that predicted by the higherredshift Supernova Legacy Survey (SNLS) supernova data for Λ colddark matter cosmologies, but does require slightly stronger cosmologicalacceleration at a low redshift. If we force the cosmological model to beflat with constant w, then we find Ω&lt;sub&gt;m&lt;/sub&gt; = 0.249 +/- 0.018and w = -1.004 +/- 0.089 after combining with the SNLS data, andincluding the WMAP measurement of the apparent acoustic horizon angle inthe cosmic microwave background.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0705.3323</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alex S.</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Measuring the Matter Density Using Baryon Oscillations in the SDSS</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...657...51P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">657</style></volume><pages><style face="normal" font="default" size="100%">51-55</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We measure the cosmological matter density by observing the positions ofbaryon acoustic oscillations in the clustering of galaxies in the SloanDigital Sky Survey (SDSS). We jointly analyze the main galaxies and LRGsin the SDSS DR5 sample, using over half a million galaxies in total. The&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0608635</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Collister, Adrian</style></author><author><style face="normal" font="default" size="100%">Lahav, Ofer</style></author><author><style face="normal" font="default" size="100%">Blake, Chris</style></author><author><style face="normal" font="default" size="100%">Cannon, Russell</style></author><author><style face="normal" font="default" size="100%">Croom, Scott</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael</style></author><author><style face="normal" font="default" size="100%">Edge, Alastair</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Roseboom, Isaac</style></author><author><style face="normal" font="default" size="100%">Ross, Nic</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shanks, Tom</style></author><author><style face="normal" font="default" size="100%">Wake, David</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">MegaZ-LRG: a photometric redshift catalogue of one million SDSS luminous red galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.375...68C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">375</style></volume><pages><style face="normal" font="default" size="100%">68-76</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We describe the construction of MegaZ-LRG, a photometric redshiftcatalogue of over one million luminous red galaxies (LRGs) in theredshift range 0.4 &amp;lt; z &amp;lt; 0.7 with limiting magnitude i &amp;lt; 20.The catalogue is selected from the imaging data of the Sloan Digital SkySurvey (SDSS) Data Release 4. The 2dF-SDSS LRG and Quasar (2SLAQ)spectroscopic redshift catalogue of 13000 intermediate-redshift LRGsprovides a photometric redshift training set, allowing use of ANNz, aneural network-based photometric-redshift estimator. The rms photometricredshift accuracy obtained for an evaluation set selected from the 2SLAQsample is σ&lt;sub&gt;z&lt;/sub&gt; = 0.049 averaged over all galaxies, andσ&lt;sub&gt;z&lt;/sub&gt; = 0.040 for a brighter subsample (i &amp;lt; 19.0). Thecatalogue is expected to contain ~5 per cent stellar contamination. TheANNz code is used to compute a refined star/galaxy probability based ona range of photometric parameters; this allows the contaminationfraction to be reduced to 2 per cent with negligible loss of genuinegalaxies. The MegaZ-LRG catalogue is publicly available on the WorldWide Web from &lt;a href=&quot;http://www.2slaq.info&quot;&gt;http://www.2slaq.info&lt;/a&gt;.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0607630</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Riess, Adam G.</style></author><author><style face="normal" font="default" size="100%">Strolger, Louis-Gregory</style></author><author><style face="normal" font="default" size="100%">Casertano, Stefano</style></author><author><style face="normal" font="default" size="100%">Ferguson, Henry C.</style></author><author><style face="normal" font="default" size="100%">Mobasher, Bahram</style></author><author><style face="normal" font="default" size="100%">Gold, Ben</style></author><author><style face="normal" font="default" size="100%">Challis, Peter J.</style></author><author><style face="normal" font="default" size="100%">Filippenko, Alexei V.</style></author><author><style face="normal" font="default" size="100%">Jha, Saurabh</style></author><author><style face="normal" font="default" size="100%">Li, Weidong</style></author><author><style face="normal" font="default" size="100%">Tonry, John</style></author><author><style face="normal" font="default" size="100%">Foley, Ryan</style></author><author><style face="normal" font="default" size="100%">Kirshner, Robert P.</style></author><author><style face="normal" font="default" size="100%">Dickinson, Mark</style></author><author><style face="normal" font="default" size="100%">MacDonald, Emily</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Livio, Mario</style></author><author><style face="normal" font="default" size="100%">Younger, Josh</style></author><author><style face="normal" font="default" size="100%">Xu, Chun</style></author><author><style face="normal" font="default" size="100%">Dahlén, Tomas</style></author><author><style face="normal" font="default" size="100%">Stern, Daniel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">New Hubble Space Telescope Discoveries of Type Ia Supernovae at z &gt;= 1: Narrowing Constraints on the Early Behavior of Dark Energy</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...659...98R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">659</style></volume><pages><style face="normal" font="default" size="100%">98-121</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We have discovered 21 new Type Ia supernovae (SNe Ia) with the HubbleSpace Telescope (HST) and have used them to trace the history of cosmicexpansion over the last 10 billion yr. These objects, which include 13spectroscopically confirmed SNe Ia at z&amp;gt;=1, were discovered during 14epochs of reimaging of the GOODS fields North and South over 2 yr withthe Advanced Camera for Surveys on  HST. Together with a recalibrationof our previous HST-discovered SNe Ia, the full sample of 23 SNe Ia atz&amp;gt;=1 provides the highest redshift sample known. Combining these datawith previous SN Ia data sets, we measured H(z) at discrete,&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0611572</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Fan, X.</style></author><author><style face="normal" font="default" size="100%">Rieke, M.</style></author><author><style face="normal" font="default" size="100%">Kennicutt, R.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">NICMOS measurements of the near-infrared background</style></title><secondary-title><style face="normal" font="default" size="100%">Nuovo Cimento B Serie</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007NCimB.122..941T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">122</style></volume><pages><style face="normal" font="default" size="100%">941-946</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present preliminary results of an ESO-VLT large programme (AMAZE)aimed at determining the evolution of the mass-metallicity relation atz~3 by means of deep near-IR spectroscopy. Gas metallicities and stellarmasses are measured for an initial sample of nine star forming galaxiesat z~3.3. When compared with previous surveys, the mass-metallicityrelation inferred at z~3.3 shows an evolution significantly strongerthan observed at lower redshifts. There are also some indications thatthe metallicity evolution of low mass galaxies is stronger relative tohigh mass systems, an effect which can be considered as the chemicalversion of the galaxy downsizing. The mass-metallicity relation observedat z~3.3 is difficult to reconcile with the predictions of somehierarchical evolutionary models. We shortly discuss the possibleimplications of such discrepancies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:0712.2880</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Sadler, Elaine M.</style></author><author><style face="normal" font="default" size="100%">Cannon, Russell D.</style></author><author><style face="normal" font="default" size="100%">Mauch, Tom</style></author><author><style face="normal" font="default" size="100%">Hancock, Paul J.</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Ross, Nic</style></author><author><style face="normal" font="default" size="100%">Croom, Scott M.</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael J.</style></author><author><style face="normal" font="default" size="100%">Edge, Alastair C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hopkins, Andrew M.</style></author><author><style face="normal" font="default" size="100%">Johnston, Helen M.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin A.</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Roseboom, Isaac G.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shanks, Tom</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Radio galaxies in the 2SLAQ Luminous Red Galaxy Survey - I. The evolution of low-power radio galaxies to z ~ 0.7</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.381..211S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">381</style></volume><pages><style face="normal" font="default" size="100%">211-227</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We have combined optical data from the 2dF-SDSS (Sloan Digital SkySurvey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ)redshift survey with radio measurements from the 1.4GHz VLA (Very LargeArray) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAOVLA Sky Survey) surveys to identify a volume-limited sample of 391 radiogalaxies at redshift 0.4 &amp;lt; z &amp;lt; 0.7. By determining an accurateradio luminosity function for luminous early-type galaxies in thisredshift range, we can investigate the cosmic evolution of theradio-galaxy population over a wide range in radio luminosity.The low-power radio galaxies in our LRG sample (those with 1.4GHz radioluminosities in the range 10&lt;sup&gt;24&lt;/sup&gt; to10&lt;sup&gt;25&lt;/sup&gt;WHz&lt;sup&gt;-1&lt;/sup&gt;, corresponding to Fanaroff-Riley I (FRI)radio galaxies in the local Universe) undergo significant cosmicevolution over the redshift range 0 &amp;lt; z &amp;lt; 0.7, consistent withpure luminosity evolution of the form (1 + z)&lt;sup&gt;k&lt;/sup&gt;, where k = 2.0+/- 0.3. Our results appear to rule out (at the 6-7σ level) modelsin which low-power radio galaxies undergo no cosmic evolution. The mostpowerful radio galaxies in our sample (with radio luminosities above10&lt;sup&gt;26&lt;/sup&gt;WHz&lt;sup&gt;-1&lt;/sup&gt;) may undergo more rapid evolution overthe same redshift range.The evolution seen in the low-power radio-galaxy population implies thatthe total energy input into massive early-type galaxies from activegalactic nucleus (AGN) heating increases with redshift, and was at least50 per cent higher at z ~ 0.55 (the median redshift of the 2SLAQ LRGsample) than in the local universe.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0612019</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A robust estimator of the small-scale galaxy correlation function</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.376.1702P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">376</style></volume><pages><style face="normal" font="default" size="100%">1702-1706</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a new estimator, ω, of the small-scale galaxycorrelation function that is robust against the effects ofredshift-space distortions and large-scale structures. The estimator isa weighted integral of the redshift space or angular correlationfunction and is a convolution of the real-space correlation functionwith a localized filter. This allows a direct comparison with theory,without modelling redshift-space distortions and the large-scalecorrelation function. This has a number of advantages over the moretraditional w&lt;sub&gt;p&lt;/sub&gt; estimator, including (i) an insensitivity tolarge-scale structures and the details of the truncation of theline-of-sight integral, (ii) a well-localized kernel in ξ(r) and(iii) being unbinned. We discuss how this estimator would be used inpractice, applying it to a sample of mock galaxies selected from theMillennium simulation.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0612103</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...664..660E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">664</style></volume><pages><style face="normal" font="default" size="100%">660-674</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We discuss the effects of nonlinear structure formation on the signatureof acoustic oscillations in the late-time galaxy distribution. We arguethat the dominant nonlinear effect is the differential motion of pairsof tracers separated by 150 Mpc. These motions are driven by bulk flowsand cluster formation and are much smaller than the acoustic scaleitself. We present a model for the nonlinear evolution based on thedistribution of pairwise Lagrangian displacements that provides aquantitative model for the degradation of the acoustic signature, evenfor biased tracers in redshift space. The Lagrangian displacementdistribution can be calibrated with a significantly smaller set ofsimulations than would be needed to construct a precise power spectrum.By connecting the acoustic signature in the Fourier basis with that inthe configuration basis, we show that the acoustic signature is morerobust than the usual Fourier-space intuition would suggest, because thebeat frequency between the peaks and troughs of the acousticoscillations is a very small wavenumber that is well inside the linearregime. We argue that any possible shift of the acoustic scale is&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0604361</style></custom3><reprint-edition><style face="normal" font="default" size="100%">systematic bias.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alex S.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Shape of the Sloan Digital Sky Survey Data Release 5 Galaxy Power Spectrum</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007ApJ...657..645P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">657</style></volume><pages><style face="normal" font="default" size="100%">645-663</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a Fourier analysis of the clustering of galaxies in thecombined main galaxy and LRG SDSS DR5 sample. The aim of our analysis isto consider how well we can measure the cosmological matter densityusing the signature of the horizon at matter-radiation equality embeddedin the large-scale power spectrum. The new data constrain the powerspectrum on scales 100-600 h&lt;sup&gt;-1&lt;/sup&gt; Mpc with significantly higherprecision than previous analyses of just the SDSS main galaxies, due toour larger sample and the inclusion of the LRGs. This improvement meansthat we can now reveal a discrepancy between the shape of the measuredpower and linear CDM models on scales 0.01 hMpc&lt;sup&gt;-1&lt;/sup&gt;-1, with linear model fitsfavoring a lower matter density (Ω&lt;sub&gt;M&lt;/sub&gt;=0.22+/-0.04) onscales 0.01 h Mpc&lt;sup&gt;-1&lt;/sup&gt;-1 and ahigher matter density (Ω&lt;sub&gt;M&lt;/sub&gt;=0.32+/-0.01) when smallerscales are included, assuming a flat ΛCDM model with h=0.73 andn&lt;sub&gt;s&lt;/sub&gt;=0.96. This discrepancy could be explained byscale-dependent bias, and by analyzing subsamples of galaxies, we findthat the ratio of small-scale to large-scale power increases with galaxyluminosity, so all of the SDSS galaxies cannot trace the same powerspectrum shape over 0.01 h Mpc&lt;sup&gt;-1&lt;/sup&gt;-1. However, the data are insufficient to clearly show aluminosity-dependent change in the largest scale at which a significantincrease in clustering is observed, although they do not rule out suchan effect. Significant scale-dependent galaxy bias on large scales,which changes with the r-band luminosity of the galaxies, couldpotentially explain differences in our Ω&lt;sub&gt;M&lt;/sub&gt; estimates anddifferences previously observed between 2dFGRS and SDSS power spectraand the resulting parameter constraints.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0608636</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kulkarni, Gauri V.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gray, Alexander</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The three-point correlation function of luminous red galaxies in the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007MNRAS.378.1196K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">378</style></volume><pages><style face="normal" font="default" size="100%">1196-1206</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present measurements of the redshift-space three-point correlationfunction of 50967 luminous red galaxies (LRGs) from Data Release 3 (DR3)of the Sloan Digital Sky Survey (SDSS). We have studied the shapedependence of the reduced three-point correlation function(Q&lt;sub&gt;z&lt;/sub&gt;(s, q, θ)) on three different scales, s = 4, 7 and10h&lt;sup&gt;-1&lt;/sup&gt;Mpc, and over the range of 1 &amp;lt; q &amp;lt; 3 and 0°&amp;lt; θ &amp;lt; 180°. On small scales (s = 4h&lt;sup&gt;-1&lt;/sup&gt;Mpc),Q&lt;sub&gt;z&lt;/sub&gt; is nearly constant, with little change as a function of qand θ. However, there is evidence for a shallow U-shapedbehaviour (with θ) which is expected from theoretical modellingof Q&lt;sub&gt;z&lt;/sub&gt;(s, q, θ). On larger scales (s = 7 and10h&lt;sup&gt;-1&lt;/sup&gt;Mpc), the U-shaped anisotropy in Q&lt;sub&gt;z&lt;/sub&gt; (withθ) is more clearly detected. We compare this shape dependence inQ&lt;sub&gt;z&lt;/sub&gt;(s, q, θ) with that seen in mock galaxy catalogueswhich were generated by populating the dark matter haloes in largeN-body simulations with mock galaxies using various halo occupationdistributions (HOD). We find that the combination of the observed numberdensity of LRGs, the (redshift-space) two-point correlation function andQ&lt;sub&gt;z&lt;/sub&gt;(s, q, θ) provides a strong constraint on theallowed HOD parameters (M&lt;sub&gt;min&lt;/sub&gt;, M&lt;sub&gt;1&lt;/sub&gt;,α) andbreaks key degeneracies between these parameters. For example, ourobserved Q&lt;sub&gt;z&lt;/sub&gt;(s, q, θ) disfavours mock catalogues thatoverpopulate massive dark matter haloes with many LRG satellites. Wealso estimate the linear bias of LRGs to be b = 1.87 +/- 0.07 inexcellent agreement with other measurements.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0703340</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Castanheira, B. G.</style></author><author><style face="normal" font="default" size="100%">Kepler, S. O.</style></author><author><style face="normal" font="default" size="100%">Costa, A. F. M.</style></author><author><style face="normal" font="default" size="100%">Giovannini, O.</style></author><author><style face="normal" font="default" size="100%">Robinson, E. L.</style></author><author><style face="normal" font="default" size="100%">Winget, D. E.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, A.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Koester, D.</style></author><author><style face="normal" font="default" size="100%">Santos, M. G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Towards a pure ZZ Ceti instability strip</style></title><secondary-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2007</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2007A%26A...462..989C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">462</style></volume><pages><style face="normal" font="default" size="100%">989-993</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Context: We have observed again two stars inside the ZZ Ceti instabilitystrip that were previously classified as not-observed-to-vary (NOV) byMukadam et al. (2004) and found them to be low-amplitude variables. Someevidence points to a pure ZZ Ceti instability strip; other evidencecontests it.  &lt;br /&gt;Aims: The two stars previously classified as NOVhave Sloan Digital Sky Survey (SDSS) spectroscopic effectivetemperatures that place them inside the ZZ Ceti instability strip, andthey were &quot;contaminating&quot; the strip as constant stars, which couldindicate that the instability strip was no longer a simple evolutionarystage. A pure instability strip indicates that pulsation is a normalphase which all DAs must go through.  &lt;br /&gt;Methods: We used effectivetemperatures derived from SDSS optical spectra by comparing them withmodel atmospheres to look for pulsators through time-resolved photometryand stars previously classified as NOV.  &lt;br /&gt;Results: Our new resultsindicate, but do not prove, a pure instability strip, because there arestill other NOV stars that need to be observed again. Additionally, wehave discovered five other ZZ Ceti stars based on their effectivetemperatures.Partially based on observations at Observatório do Pico dosDias/LNA; the Southern Astrophysical Research telescope, a collaborationbetween CNPq-Brazil, NOAO, UNC, and MSU; and McDonald Observatory of TheUniversity of Texas at Austin.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0611332</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Edge, Alastair C.</style></author><author><style face="normal" font="default" size="100%">Cannon, Russell</style></author><author><style face="normal" font="default" size="100%">Smail, Ian</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Carson, Daniel</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas P.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Colless, Matthew</style></author><author><style face="normal" font="default" size="100%">Couch, Warrwick J.</style></author><author><style face="normal" font="default" size="100%">Croom, Scott M.</style></author><author><style face="normal" font="default" size="100%">Driver, Simon P.</style></author><author><style face="normal" font="default" size="100%">da Ângela, José</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael J.</style></author><author><style face="normal" font="default" size="100%">Bland-Hawthorn, Joss</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin A.</style></author><author><style face="normal" font="default" size="100%">Roseboom, Isaac G.</style></author><author><style face="normal" font="default" size="100%">Shanks, Tom</style></author><author><style face="normal" font="default" size="100%">Sharp, Robert G.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The 2df SDSS LRG and QSO survey: evolution of the luminosity function of luminous red galaxies to z = 0.6</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006MNRAS.372..537W</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">372</style></volume><pages><style face="normal" font="default" size="100%">537-550</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present new measurements of the luminosity function (LF) of luminousred galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) and the 2dFSDSS LRG and Quasar (2SLAQ) survey. We have carefully quantified, andcorrected for, uncertainties in the K and evolutionary corrections,differences in the colour selection methods, and the effects ofphotometric errors, thus ensuring we are studying the same galaxypopulation in both surveys. Using a limited subset of 6326 SDSS LRGs(with 0.17 &amp;lt; z &amp;lt; 0.24) and 1725 2SLAQ LRGs (with 0.5 &amp;lt; z &amp;lt;0.6), for which the matching colour selection is most reliable, we findno evidence for any additional evolution in the LRG LF, over thisredshift range, beyond that expected from a simple passive evolutionmodel. This lack of additional evolution is quantified using thecomoving luminosity density of SDSS and 2SLAQ LRGs, brighter thanM&lt;sub&gt;0.2&lt;/sub&gt;&lt;sub&gt;r&lt;/sub&gt; - 5 log h&lt;sub&gt;0.7&lt;/sub&gt; = -22.5, which are2.51 +/- 0.03 × 10&lt;sup&gt;-7&lt;/sup&gt;L&lt;sub&gt;solar&lt;/sub&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;and 2.44 +/- 0.15 ×10&lt;sup&gt;-7&lt;/sup&gt;L&lt;sub&gt;solar&lt;/sub&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;, respectively (&amp;lt;10per cent uncertainty). We compare our LFs to the COMBO-17 data and findexcellent agreement over the same redshift range. Together, thesesurveys show no evidence for additional evolution (beyond passive) inthe LF of LRGs brighter than M&lt;sub&gt;0.2&lt;/sub&gt;&lt;sub&gt;r&lt;/sub&gt; - 5 logh&lt;sub&gt;0.7&lt;/sub&gt; = -21 (or brighter than ~L*). We test our SDSS and 2SLAQLFs against a simple `dry merger' model for the evolution of massive redgalaxies and find that at least half of the LRGs at z ~= 0.2 mustalready have been well assembled (with more than half their stellarmass) by z ~= 0.6. This limit is barely consistent with recent resultsfrom semi-analytical models of galaxy evolution.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0607629</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Cannon, Russell</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael</style></author><author><style face="normal" font="default" size="100%">Edge, Alastair</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert</style></author><author><style face="normal" font="default" size="100%">Outram, Phillip</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Roseboom, Isaac</style></author><author><style face="normal" font="default" size="100%">Wake, David</style></author><author><style face="normal" font="default" size="100%">Allen, Paul</style></author><author><style face="normal" font="default" size="100%">Bland-Hawthorn, Joss</style></author><author><style face="normal" font="default" size="100%">Bridges, Terry</style></author><author><style face="normal" font="default" size="100%">Carson, Daniel</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Colless, Matthew</style></author><author><style face="normal" font="default" size="100%">Couch, Warrick</style></author><author><style face="normal" font="default" size="100%">Croom, Scott</style></author><author><style face="normal" font="default" size="100%">Driver, Simon</style></author><author><style face="normal" font="default" size="100%">Fine, Stephen</style></author><author><style face="normal" font="default" size="100%">Hewett, Paul</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Ross, Nicholas</style></author><author><style face="normal" font="default" size="100%">Sadler, Elaine M.</style></author><author><style face="normal" font="default" size="100%">Shanks, Tom</style></author><author><style face="normal" font="default" size="100%">Sharp, Robert</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Weilbacher, Peter</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The 2dF-SDSS LRG and QSO (2SLAQ) Luminous Red Galaxy Survey</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006MNRAS.372..425C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">372</style></volume><pages><style face="normal" font="default" size="100%">425-442</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a spectroscopic survey of almost 15000 candidateintermediate-redshift luminous red galaxies (LRGs) brighter than i =19.8, observed with 2dF on the Anglo-Australian Telescope. The targetswere selected photometrically from the Sloan Digital Sky Survey (SDSS)and lie along two narrow equatorial strips covering 180 deg&lt;sup&gt;2&lt;/sup&gt;.Reliable redshifts were obtained for 92 per cent of the targets and theselection is very efficient: over 90 per cent have 0.45 &amp;lt; z &amp;lt; 0.8.More than 80 per cent of the ~11000 red galaxies have pureabsorption-line spectra consistent with a passively evolving old stellarpopulation. The redshift, photometric and spatial distributions of theLRGs are described. The 2SLAQ data will be released publicly frommid-2006, providing a powerful resource for observational cosmology andthe study of galaxy evolution.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0607631</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Roseboom, Isaac G.</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin A.</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael J.</style></author><author><style face="normal" font="default" size="100%">Cannon, Russell D.</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Edge, Alastair C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Smail, Ian</style></author><author><style face="normal" font="default" size="100%">Wake, David A.</style></author><author><style face="normal" font="default" size="100%">Bland-Hawthorn, Joss</style></author><author><style face="normal" font="default" size="100%">Bridges, Terry J.</style></author><author><style face="normal" font="default" size="100%">Carson, Daniel</style></author><author><style face="normal" font="default" size="100%">Colless, Matthew</style></author><author><style face="normal" font="default" size="100%">Couch, Warrick J.</style></author><author><style face="normal" font="default" size="100%">Croom, Scott M.</style></author><author><style face="normal" font="default" size="100%">Driver, Simon P.</style></author><author><style face="normal" font="default" size="100%">Hewett, Paul C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Ross, Nic</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shanks, Tom</style></author><author><style face="normal" font="default" size="100%">Sharp, Robert G.</style></author><author><style face="normal" font="default" size="100%">Weilbacher, Peter</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The 2dF-SDSS LRG and QSO Survey: the star formation histories of luminous red galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006MNRAS.373..349R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">373</style></volume><pages><style face="normal" font="default" size="100%">349-360</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a detailed investigation into the recent star formationhistories of 5697 luminous red galaxies (LRGs) based on the Hδ(4101 Å), and [OII] (3727 Å) lines and the D4000 index. LRGsare luminous (L &amp;gt; 3L*) galaxies which have been selected to havephotometric properties consistent with an old, passively evolvingstellar population. For this study, we utilize LRGs from the recentlycompleted 2dF-SDSS LRG and QSO Survey (2SLAQ). Equivalent widths of theHδ and [OII] lines are measured and used to define three spectraltypes, those with only strong Hδ absorption (k+a), those withstrong [OII] in emission (em) and those with both (em+a). All other LRGsare considered to have passive star formation histories. The vastmajority of LRGs are found to be passive (~80 per cent); however,significant numbers of k+a (2.7 per cent), em+a (1.2 per cent) and emLRGs (8.6 per cent) are identified. An investigation into the redshiftdependence of the fractions is also performed. A sample of SDSS MAINgalaxies with colours and luminosities consistent with the 2SLAQ LRGs isselected to provide a low-redshift comparison. While the em and em+afractions are consistent with the low-redshift SDSS sample, the fractionof k+a LRGs is found to increase significantly with redshift. Thisresult is interpreted as an indication of an increasing amount of recentstar formation activity in LRGs with redshift. By considering theexpected lifetime of the k+a phase, the number of LRGs which willundergo a k+a phase can be estimated. A crude comparison of thisestimate with the predictions from semi-analytic models of galaxyformation shows that the predicted level of k+a and em+a activities isnot sufficient to reconcile the predicted mass growth for massive earlytypes in a hierarchical merging scenario.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0609178</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kollmeier, Juna A.</style></author><author><style face="normal" font="default" size="100%">Onken, Christopher A.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Gould, Andrew</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Dietrich, Matthias</style></author><author><style face="normal" font="default" size="100%">Cool, Richard</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Le Floc'h, Emeric</style></author><author><style face="normal" font="default" size="100%">Stern, Daniel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Black Hole Masses and Eddington Ratios at 0.3 &lt; z &lt; 4</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...648..128K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">648</style></volume><pages><style face="normal" font="default" size="100%">128-139</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We study the distribution of Eddington luminosity ratios,L&lt;sub&gt;bol&lt;/sub&gt;/L&lt;sub&gt;Edd&lt;/sub&gt;, of active galactic nuclei (AGNs)discovered in the AGN and Galaxy Evolution Survey (AGES). We combineHβ, Mg II, and C IV line widths with continuum luminosities toestimate black hole (BH) masses in 407 AGNs, covering the redshift rangez~0.3-4 and the bolometric luminosity rangeL&lt;sub&gt;bol&lt;/sub&gt;~10&lt;sup&gt;45&lt;/sup&gt;-10&lt;sup&gt;47&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. Thesample consists of X-ray or mid-infrared (24 μm) point sources withoptical magnitude R&amp;lt;=21.5 mag and optical emission-line spectracharacteristic of AGNs. For the range of luminosity and redshift probedby AGES, the distribution of estimated Eddington ratios is welldescribed as log-normal, with a peak atL&lt;sub&gt;bol&lt;/sub&gt;/L&lt;sub&gt;Edd&lt;/sub&gt;~=1/4 and a dispersion of 0.3 dex. Sinceadditional sources of scatter are minimal, this dispersion must accountfor contributions from the scatter between estimated and true BH massand the scatter between estimated and true bolometric luminosity.Therefore, we conclude that (1) neither of these sources of error cancontribute more than ~0.3 dex rms, and (2) the true Eddington ratios ofoptically luminous AGNs are even more sharply peaked. Because the massestimation errors must be smaller than ~0.3 dex, we can also investigatethe distribution of Eddington ratios at fixed BH mass. We show for thefirst time that the distribution of Eddington ratios at fixed BH mass ispeaked, and that the dearth of AGNs at a factor of ~10 below Eddingtonis real and not an artifact of sample selection. These results providestrong evidence that supermassive BHs gain most of their mass whileradiating close to the Eddington limit, and they suggest that thefueling rates in luminous AGNs are ultimately determined by BHself-regulation of the accretion flow rather than galactic-scaledynamical disturbances.Observations reported here were obtained at the MMT Observatory (MMTO),a joint facility of the University of Arizona and the SmithsonianInstitution.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0508657</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Broadband Optical Properties of Massive Galaxies: The Dispersion around the Field Galaxy Color-Magnitude Relation Out to z~0.4</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131..736C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">736-746</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Using a sample of nearly 20,000 massive early-type galaxies selectedfrom the Sloan Digital Sky Survey, we study the color-magnitude relationfor the most luminous (L&amp;gt;~2.2L&lt;sup&gt;*&lt;/sup&gt;) field galaxies in theredshift range 0.1&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0510301</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott A.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Long, Dan</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Catalog of Spectroscopically Confirmed White Dwarfs from the Sloan Digital Sky Survey Data Release 4</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJS..167...40E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">167</style></volume><pages><style face="normal" font="default" size="100%">40-58</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a catalog of 9316 spectroscopically confirmed white dwarfsfrom the Sloan Digital Sky Survey Data Release 4. We have selected thestars through photometric cuts and spectroscopic modeling, backed up bya set of visual inspections. About 6000 of the stars are newdiscoveries, roughly doubling the number of spectroscopically confirmedwhite dwarfs. We analyze the stars by performing temperature and surfacegravity fits to grids of pure hydrogen and helium atmospheres. Among therare outliers are a set of presumed helium-core DA white dwarfs withestimated masses below 0.3 M&lt;sub&gt;solar&lt;/sub&gt;, including two candidatesthat may be the lowest-mass yet found. We also present a list of 928 hotsubdwarfs.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0606700</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine</style></author><author><style face="normal" font="default" size="100%">Schmidt, Gary D.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Wolfe, Michael A.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Kleinman, Scot J.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, John</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Long, Dan</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Catalog of Spectroscopically Selected Close Binary Systems from the Sloan Digital Sky Survey Data Release Four</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131.1674S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">1674-1686</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a spectroscopic sample of 747 detached close binary systemsfrom the Sloan Digital Sky Survey (SDSS) Fourth Data Release. Themajority of these binaries consist of a white dwarf primary and alow-mass secondary (typically M dwarf) companion. We have determined thetemperature and gravity for 496 of the white dwarf primaries and thespectral type and magnetic activity properties for 661 of the low-masssecondaries. We have estimated the distances for each of the whitedwarf-main-sequence star binaries and use white dwarf evolutionary gridsto establish the age of each binary system from the white dwarf coolingtimes. With respect to a spectroscopically identified sample of ~8000isolated M dwarf stars in the SDSS, the M dwarf secondaries showenhanced activity with a higher active fraction at a given spectraltype. The white dwarf temperatures and gravities are similar to thedistribution of ~1900 DA white dwarfs from the SDSS. The ages of thebinaries in this study range from ~0.5 Myr to nearly 3 Gyr (average age~0.20 Gyr).&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1086/499494</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ota, Naomi</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Mitsuda, Kazuhisa</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Suto, Yasushi</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Fujimoto, Ryuichi</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">Minezaki, Takeo</style></author><author><style face="normal" font="default" size="100%">Yoshii, Yuzuru</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Chandra Observations of SDSS J1004+4112: Constraints on the Lensing Cluster and Anomalous X-Ray Flux Ratios of the Quadruply Imaged Quasar</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...647..215O</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">647</style></volume><pages><style face="normal" font="default" size="100%">215-221</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present results from Chandra observations of SDSS J1004+4112, astrongly lensed quasar system with a maximum image separation of 15&quot;.All four bright images of the quasar, as well as resolved X-ray emissionoriginating from the lensing cluster, are clearly detected. The emissionfrom the lensing cluster extends out to approximately 1.5 arcmin. Wemeasure the bolometric X-ray luminosity and temperature of the lensingcluster to be 4.7×10&lt;sup&gt;44&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and 6.4 keV,consistent with the luminosity-temperature relation for distantclusters. The mass estimated from the X-ray observation shows excellentagreement with the mass derived from gravitational lensing. The X-rayflux ratios of the quasar images differ markedly from the optical fluxratios, and the combined X-ray spectrum of the images possesses anunusually strong Fe Kα emission line, both of which are indicativeof microlensing.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0601700</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hamilton, Andrew J. S.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Percival, Will J.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Swanson, Molly</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Yoo, Jaiyul</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Abazajian, Kevork</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bassett, Bruce</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Budavari, Tamás</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Pan, Kaike</style></author><author><style face="normal" font="default" size="100%">Park, Changbom</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Cosmological constraints from the SDSS luminous red galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">Physical Review D</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006PhRvD..74l3507T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">74</style></volume><pages><style face="normal" font="default" size="100%">123507</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We measure the large-scale real-space power spectrum P(k) using luminousred galaxies (LRGs) in the Sloan Digital Sky Survey (SDSS) and use thismeasurement to sharpen constraints on cosmological parameters from theWilkinson Microwave Anisotropy Probe (WMAP). We employ a matrix-basedpower spectrum estimation method using Pseudo-Karhunen-Loèveeigenmodes, producing uncorrelated minimum-variance measurements in 20k-bands of both the clustering power and its anisotropy due toredshift-space distortions, with narrow and well-behaved windowfunctions in the range 0.01h/Mpcm and the baryon fraction in goodagreement with WMAP. Within the context of flat ΛCDM models, ourLRG measurements complement WMAP by sharpening the constraints on thematter density, the neutrino density and the tensor amplitude by about afactor of 2, giving Ω&lt;sub&gt;m&lt;/sub&gt;=0.24±0.02 (1σ),&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0608632</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Castanheira, B. G.</style></author><author><style face="normal" font="default" size="100%">Kepler, S. O.</style></author><author><style face="normal" font="default" size="100%">Mullally, F.</style></author><author><style face="normal" font="default" size="100%">Winget, D. E.</style></author><author><style face="normal" font="default" size="100%">Koester, D.</style></author><author><style face="normal" font="default" size="100%">Voss, B.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, A.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Napiwotzki, R.</style></author><author><style face="normal" font="default" size="100%">Reimers, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Discovery of eleven new ZZ Ceti stars</style></title><secondary-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006A%26A...450..227C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">450</style></volume><pages><style face="normal" font="default" size="100%">227-231</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of eleven new ZZ Cetis using telescopes at OPD(Observatório do Pico dos Dias/LNA) in Brazil, the 4.1 m SOAR(Southern Astrophysical Research) telescope at Cerro Pachon, Chile, andthe 2.1 m Otto Struve telescope at McDonald observatory. The candidateswere selected from the SDSS (Sloan Digital Sky Survey) and SPY (ESO SNIa progenitor survey), based on their T&lt;sub&gt;eff&lt;/sub&gt; obtained fromoptical spectra fitting. This selection criterion yields the highest&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0511804</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Stern, Daniel</style></author><author><style face="normal" font="default" size="100%">Brand, Kate</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, Peter R.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Gonzalez, Anthony H.</style></author><author><style face="normal" font="default" size="100%">Green, Richard F.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">McKenzie, Eric H.</style></author><author><style face="normal" font="default" size="100%">Rieke, George H.</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia</style></author><author><style face="normal" font="default" size="100%">Soifer, Baruch T.</style></author><author><style face="normal" font="default" size="100%">Spinrad, Hyron</style></author><author><style face="normal" font="default" size="100%">Elston, Richard J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Discovery of Three New z&gt;5 Quasars in the AGN and Galaxy Evolution Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....132..823C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">132</style></volume><pages><style face="normal" font="default" size="100%">823-830</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the discovery of three z&amp;gt;5 quasars in the AGN and GalaxyEvolution Survey spectroscopic observations of the NOAO Deep Wide-FieldSurvey (NDWFS) Bootes Field. These quasars were selected as part of alarger Spitzer mid-infrared quasar sample, with no selection based onoptical colors. The highest redshift object, NDWFS J142516.3+325409, atz=5.85, is the lowest luminosity z&amp;gt;5.8 quasar currently known. Wecompare mid-infrared techniques for identifying z&amp;gt;5 quasars to moretraditional optical techniques and show that mid-infrared colors allowfor the selection of high-redshift quasars even at redshifts at whichquasars lie near the optical stellar locus and at z&amp;gt;7, where opticalselection is impossible. Using the superb multiwavelength coverageavailable in the NDWFS Bootes field, we construct the spectral energydistributions (SEDs) of high-redshift quasars from observedB&lt;sub&gt;W&lt;/sub&gt; band to 24 μm (rest-frame 600 Å-3.7 μm). Weshow that the three high-redshift quasars have quite similar SEDs, andthe rest-frame composite SED of low-redshift quasars from the literatureshows little evolution compared to our high-redshift objects. We comparethe number of z&amp;gt;5 quasars we have discovered to the expected numberfrom published quasar luminosity functions. While analyses of the quasarluminosity function are tenuous based on only three objects, we findthat a relatively steep luminosity function with Ψ~L&lt;sup&gt;-3.2&lt;/sup&gt;provides the best agreement with the number of high-redshift quasarsdiscovered in our survey.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0605030</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Anderson, Kurt S. J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinchmann, Jarle</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carey, Larry N.</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Czarapata, Paul C.</style></author><author><style face="normal" font="default" size="100%">Dalcanton, Julianne J.</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Dong, Feng</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Gurbani, Vijay K.</style></author><author><style face="normal" font="default" size="100%">de Haas, Ernst</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Harris, Frederick H.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hayes, Jeffrey</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hirata, Christopher M.</style></author><author><style face="normal" font="default" size="100%">Hogan, Craig J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holmgren, Donald J.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kniazev, Alexei Yu.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Kuropatkin, Nikolay</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Martínez-Delgado, David</style></author><author><style face="normal" font="default" size="100%">Mandelbaum, Rachel</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Nash, Thomas</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">O'Mullane, William</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Pauls, George</style></author><author><style face="normal" font="default" size="100%">Peoples, John, Jr.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Pourbaix, Dimitri</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas R.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schroeder, Joshua</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Walkowicz, Lucianne M.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Xu, Yongzhong</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zibetti, Stefano</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Fourth Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Supplement Series</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJS..162...38A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">162</style></volume><pages><style face="normal" font="default" size="100%">38-48</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper describes the Fourth Data Release of the Sloan Digital SkySurvey (SDSS), including all survey-quality data taken through 2004June. The data release includes five-band photometric data for 180million objects selected over 6670 deg&lt;sup&gt;2&lt;/sup&gt; and 673,280 spectraof galaxies, quasars, and stars selected from 4783 deg&lt;sup&gt;2&lt;/sup&gt; ofthose imaging data using the standard SDSS target selection algorithms.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0507711</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Koester, Detlev</style></author><author><style face="normal" font="default" size="100%">Kleinmann, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Smith, Paul S.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Long, Dan</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Hot DB White Dwarfs from the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....132..676E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">132</style></volume><pages><style face="normal" font="default" size="100%">676-691</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present ugriz photometry and optical spectroscopy for 28 DB and DOwhite dwarfs with temperatures between 28,000 and 45,000 K. About 10 ofthese are particularly well observed; the remainder are candidates.These are the hottest DB stars yet found, and they populate the ``DBgap'' between the hotter DO stars and the familiar DB stars cooler than30,000 K. Nevertheless, after carefully matching the survey volumes wefind that the ratio of DA stars to DB stars is a factor of 2.5 larger at30,000 than at 20,000 K, suggesting that the ``DB gap'' is indeeddeficient and that some kind of atmospheric transformation takes place&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0606702</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Papovich, Casey</style></author><author><style face="normal" font="default" size="100%">Cool, Richard</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Le Floc'h, Emeric</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Kennicutt, Robert C., Jr.</style></author><author><style face="normal" font="default" size="100%">Smith, J. D. T.</style></author><author><style face="normal" font="default" size="100%">Rieke, G. H.</style></author><author><style face="normal" font="default" size="100%">Vestergaard, Marianne</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">An MMT Hectospec Redshift Survey of 24 μm Sources in the Spitzer First Look Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....132..231P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">132</style></volume><pages><style face="normal" font="default" size="100%">231-241</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a spectroscopic survey using the MMT Hectospec fiberspectrograph of 24 μm sources selected with the Spitzer SpaceTelescope in the Spitzer First Look Survey. We report 1296 new redshiftsfor 24 μm sources, including 599 with f&lt;sub&gt;ν&lt;/sub&gt;(24μm)&amp;gt;=1 mJy. Combined with 291 additional redshifts for sourcesfrom the Sloan Digital Sky Survey (SDSS), our observing program was&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0512623</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Brodwin, M.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Ashby, M. L. N.</style></author><author><style face="normal" font="default" size="100%">Bian, C.</style></author><author><style face="normal" font="default" size="100%">Brand, K.</style></author><author><style face="normal" font="default" size="100%">Dey, A.</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, P. R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Gonzalez, A. H.</style></author><author><style face="normal" font="default" size="100%">Huang, J.-S.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Kochanek, C. S.</style></author><author><style face="normal" font="default" size="100%">McKenzie, E.</style></author><author><style face="normal" font="default" size="100%">Murray, S. S.</style></author><author><style face="normal" font="default" size="100%">Pahre, M. A.</style></author><author><style face="normal" font="default" size="100%">Smith, H. A.</style></author><author><style face="normal" font="default" size="100%">Soifer, B. T.</style></author><author><style face="normal" font="default" size="100%">Stanford, S. A.</style></author><author><style face="normal" font="default" size="100%">Stern, D.</style></author><author><style face="normal" font="default" size="100%">Elston, R. J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Photometric Redshifts in the IRAC Shallow Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...651..791B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">651</style></volume><pages><style face="normal" font="default" size="100%">791-803</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Accurate photometric redshifts are calculated for nearly 200,000galaxies to a 4.5 μm flux limit of ~13 μJy in the 8.5deg&lt;sup&gt;2&lt;/sup&gt; Spitzer IRAC Shallow Survey. Using a hybrid photometricredshift algorithm incorporating both neural net and template-fittingtechniques, calibrated with over 15,000 spectroscopic redshifts, a&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0607450</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Yang, Yujin</style></author><author><style face="normal" font="default" size="100%">Zabludoff, Ann I.</style></author><author><style face="normal" font="default" size="100%">Davé, Romeel</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Pinto, Philip A.</style></author><author><style face="normal" font="default" size="100%">Katz, Neal</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Barton, Elizabeth J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Probing Galaxy Formation with He II Cooling Lines</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...640..539Y</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">640</style></volume><pages><style face="normal" font="default" size="100%">539-552</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Using high-resolution cosmological simulations, we study hydrogen andhelium gravitational cooling radiation from gas accretion by younggalaxies. We focus on the He II cooling lines, which arise from gas witha different temperature history (T&lt;sub&gt;max&lt;/sub&gt;~10&lt;sup&gt;5&lt;/sup&gt; K) thanH I line-emitting gas. We examine whether three major atomic coolinglines, H I λ1216, He II λ1640, and He II λ304, areobservable, finding that Lyα and He II λ1640 coolingemission at z=2-3 are potentially detectable with deep narrowband(R&amp;gt;100) imaging and/or spectroscopy from the ground. While theexpected strength of H I λ1216 cooling emission depends stronglyon the treatment of the self-shielded phase of the IGM in thesimulations, our predictions for the He II λ1640 line are morerobust, because the He II emissivity is negligible belowT~10&lt;sup&gt;4.5&lt;/sup&gt; K and less sensitive to the UV background. AlthoughHe II λ1640 cooling emission is fainter than Lyα by atleast a factor of 10 and, unlike Lyα, might not be resolvedspatially with current observational facilities, it is more suitable tostudy gas accretion in the galaxy formation process because it isoptically thin and less contaminated by the recombination lines fromstar-forming galaxies. The He II λ1640 line can be used todistinguish among mechanisms for powering the so-called Lyαblobs-including gravitational cooling radiation, photoionization bystellar populations, and starburst-driven superwinds-because (1) He IIλ1640 emission is limited to very low metallicity[log(Z/Z&lt;sub&gt;solar&lt;/sub&gt;)&amp;lt;~-5.3] and Population III stars and (2) theblob's kinematics are probed unambiguously through the He II line width,which for cooling radiation is narrower (σ&amp;lt;400 kms&lt;sup&gt;-1&lt;/sup&gt;) than typical wind speeds.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0509007</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Steinmetz, M.</style></author><author><style face="normal" font="default" size="100%">Zwitter, T.</style></author><author><style face="normal" font="default" size="100%">Siebert, A.</style></author><author><style face="normal" font="default" size="100%">Watson, F. G.</style></author><author><style face="normal" font="default" size="100%">Freeman, K. C.</style></author><author><style face="normal" font="default" size="100%">Munari, U.</style></author><author><style face="normal" font="default" size="100%">Campbell, R.</style></author><author><style face="normal" font="default" size="100%">Williams, M.</style></author><author><style face="normal" font="default" size="100%">Seabroke, G. M.</style></author><author><style face="normal" font="default" size="100%">Wyse, R. F. G.</style></author><author><style face="normal" font="default" size="100%">Parker, Q. A.</style></author><author><style face="normal" font="default" size="100%">Bienaymé, O.</style></author><author><style face="normal" font="default" size="100%">Roeser, S.</style></author><author><style face="normal" font="default" size="100%">Gibson, B. K.</style></author><author><style face="normal" font="default" size="100%">Gilmore, G.</style></author><author><style face="normal" font="default" size="100%">Grebel, E. K.</style></author><author><style face="normal" font="default" size="100%">Helmi, A.</style></author><author><style face="normal" font="default" size="100%">Navarro, J. F.</style></author><author><style face="normal" font="default" size="100%">Burton, D.</style></author><author><style face="normal" font="default" size="100%">Cass, C. J. P.</style></author><author><style face="normal" font="default" size="100%">Dawe, J. A.</style></author><author><style face="normal" font="default" size="100%">Fiegert, K.</style></author><author><style face="normal" font="default" size="100%">Hartley, M.</style></author><author><style face="normal" font="default" size="100%">Russell, K. S.</style></author><author><style face="normal" font="default" size="100%">Saunders, W.</style></author><author><style face="normal" font="default" size="100%">Enke, H.</style></author><author><style face="normal" font="default" size="100%">Bailin, J.</style></author><author><style face="normal" font="default" size="100%">Binney, J.</style></author><author><style face="normal" font="default" size="100%">Bland-Hawthorn, J.</style></author><author><style face="normal" font="default" size="100%">Boeche, C.</style></author><author><style face="normal" font="default" size="100%">Dehnen, W.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Evans, N. W.</style></author><author><style face="normal" font="default" size="100%">Fiorucci, M.</style></author><author><style face="normal" font="default" size="100%">Fulbright, J. P.</style></author><author><style face="normal" font="default" size="100%">Gerhard, O.</style></author><author><style face="normal" font="default" size="100%">Jauregi, U.</style></author><author><style face="normal" font="default" size="100%">Kelz, A.</style></author><author><style face="normal" font="default" size="100%">Mijović, L.</style></author><author><style face="normal" font="default" size="100%">Minchev, I.</style></author><author><style face="normal" font="default" size="100%">Parmentier, G.</style></author><author><style face="normal" font="default" size="100%">Peñarrubia, J.</style></author><author><style face="normal" font="default" size="100%">Quillen, A. C.</style></author><author><style face="normal" font="default" size="100%">Read, M. A.</style></author><author><style face="normal" font="default" size="100%">Ruchti, G.</style></author><author><style face="normal" font="default" size="100%">Scholz, R.-D.</style></author><author><style face="normal" font="default" size="100%">Siviero, A.</style></author><author><style face="normal" font="default" size="100%">Smith, M. C.</style></author><author><style face="normal" font="default" size="100%">Sordo, R.</style></author><author><style face="normal" font="default" size="100%">Veltz, L.</style></author><author><style face="normal" font="default" size="100%">Vidrih, S.</style></author><author><style face="normal" font="default" size="100%">von Berlepsch, R.</style></author><author><style face="normal" font="default" size="100%">Boyle, B. J.</style></author><author><style face="normal" font="default" size="100%">Schilbach, E.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Radial Velocity Experiment (RAVE): First Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....132.1645S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">132</style></volume><pages><style face="normal" font="default" size="100%">1645-1668</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the first data release of the Radial Velocity Experiment(RAVE), an ambitious spectroscopic survey to measure radial velocitiesand stellar atmosphere parameters (temperature, metallicity, and surfacegravity) of up to one million stars using the Six Degree Fieldmultiobject spectrograph on the 1.2 m UK Schmidt Telescope of theAnglo-Australian Observatory. The RAVE program started in 2003,obtaining medium-resolution spectra (median R=7500) in the Ca-tripletregion (8410-8795 Å) for southern hemisphere stars drawn from theTycho-2 and SuperCOSMOS catalogs, in the magnitude range 9&lt;i&gt;2. The average signal-to-noise ratio of&lt;/i&gt;&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0606211</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Scale Dependence of Relative Galaxy Bias: Encouragement for the ``Halo Model'' Description</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...645..977B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">645</style></volume><pages><style face="normal" font="default" size="100%">977-985</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We investigate the relationship between the colors, luminosities, andenvironments of galaxies in the Sloan Digital Sky Survey spectroscopicsample, using environmental measurements on scales ranging from 0.2 to 6h&lt;sup&gt;-1&lt;/sup&gt; Mpc. We find that (1) the relationship between color andenvironment persists even to the lowest luminosities we probe(M&lt;sub&gt;r&lt;/sub&gt;-5log10h~-14) (2) at luminosities and colors for which thegalaxy correlation function has a large amplitude, it also has a steepslope; and (3) in regions of a given overdensity on small scales (1h&lt;sup&gt;-1&lt;/sup&gt; Mpc), the overdensity on large scales (6 h&lt;sup&gt;-1&lt;/sup&gt;Mpc) does not appear to relate to the recent star formation history ofthe galaxies. Of these results, the last has the most immediateapplication to galaxy formation theory. In particular, it lends supportto the notion that a galaxy's properties are related only to the mass ofits host dark matter halo, and not to the larger scale environment.Based on observations obtained with the Sloan Digital Sky Survey.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0411037</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Pindor, Bart</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">Brasi, Guido</style></author><author><style face="normal" font="default" size="100%">Hinz, Philip M.</style></author><author><style face="normal" font="default" size="100%">Kenworthy, Matthew A.</style></author><author><style face="normal" font="default" size="100%">Miller, Doug</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Long, Dan</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J102111.02+491330.4: A Newly Discovered Gravitationally Lensed Quasar</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131...41P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">41-48</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report follow-up observations of two gravitational lens candidatesidentified in the Sloan Digital Sky Survey (SDSS) data set. We haveconfirmed that SDSS J102111.02+491330.4 is a previously unknowngravitationally lensed quasar. This lens system exhibits two images of az=1.72 quasar, with an image separation of 1.14&quot;+/-0.04&quot;. Optical andnear-IR imaging of the system reveals the presence of the lensing galaxybetween the two quasar images. Observations of SDSS J112012.12+671116.0indicate that it is more likely a binary quasar than a gravitationallens. This system has two quasars at a redshift of z=1.49, with anangular separation of 1.49&quot;+/-0.02&quot;. However, the two quasars havemarkedly different spectral energy distributions, and no lens galaxy isapparent in optical and near-IR images of this system. We also present alist of 31 SDSS lens candidates that follow-up observations haveconfirmed are not gravitational lenses.Observations reported here were obtained at the MMT Observatory, a jointfacility of the University of Arizona and the Smithsonian Institution.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0509296</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy A.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Beers, Timothy C.</style></author><author><style face="normal" font="default" size="100%">Allende Prieto, Carlos</style></author><author><style face="normal" font="default" size="100%">Wilhelm, Ron</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Niederste-Ostholt, Martin</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Covey, Kevin</style></author><author><style face="normal" font="default" size="100%">Seth, Anil</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Helmboldt, Joe</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Kleinman, Scot J.</style></author><author><style face="normal" font="default" size="100%">Long, Dan</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Barentine, John C.</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nielsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J103913.70+533029.7: A Super Star Cluster in the Outskirts of a Galaxy Merger</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131..859K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">859-865</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We describe the serendipitous discovery in the spectroscopic data of theSloan Digital Sky Survey of a starlike object, SDSS J103913.70+533029.7,at a heliocentric radial velocity of +1012 km s&lt;sup&gt;-1&lt;/sup&gt;. Itsproximity in position and velocity to the spiral galaxy NGC 3310suggests an association with the galaxy. At this distance, SDSSJ103913.70+533029.7 has the luminosity of a super star cluster and aprojected distance of 17 kpc from NGC 3310. Its spectroscopic andphotometric properties imply a mass of &amp;gt;10&lt;sup&gt;6&lt;/sup&gt;M&lt;sub&gt;solar&lt;/sub&gt; and an age close to that of the tidal shells seenaround NGC 3310, suggesting that it formed in the event that formed theshells.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0511010</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS Preburst Observations of Recent Gamma-Ray Burst Fields</style></title><secondary-title><style face="normal" font="default" size="100%">Publications of the Astronomical Society of the Pacific</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006PASP..118..733C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">118</style></volume><pages><style face="normal" font="default" size="100%">733-739</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present Sloan Digital Sky Survey (SDSS) photometry and spectroscopyin the fields of 27 gamma-ray bursts observed by Swift, including burstslocalized by Swift, HETE-2, and INTEGRAL, after 2004 December. Afterthis bulk release, we plan to provide individual releases of similardata shortly after the localization of future bursts falling in the SDSSsurvey area. These data provide a solid basis for the astrometric andphotometric calibration of follow-up afterglow searches and monitoring.Furthermore, the images provided with this release will allow observersto find transient objects up to a magnitude fainter than is possiblewith Digitized Sky Survey images.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0601218</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Haiman, Zoltán</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Snapshot Survey for Gravitational Lenses among z&gt;=4.0 Quasars. II. Constraints on the 4.0&lt;z&lt;5.4 Quasar Population</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131...49R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">49-54</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report on i-band snapshot observations of 157 Sloan Digital SkySurvey quasars at 4.0-3.8 (3 σ), assuming a break in the quasar luminosityfunction at M&lt;sup&gt;*&lt;/sup&gt;&lt;sub&gt;1450&lt;/sub&gt;~-24.5. This constraint isconsiderably stronger than the limit of β&amp;gt;-4.63 obtained fromthe absence of lensing in four z&amp;gt;5.7 quasars. Such constraints areimportant to our understanding of the true space density ofhigh-redshift quasars and the ionization state of the early universe.Based on observations made with the NASA/ESA Hubble Space Telescope,obtained at the Space Telescope Science Institute, which is operated bythe Association of Universities for Research in Astronomy, Inc., underNASA contract NAS5-26555. These observations are associated with program9472.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0509135</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Jiang, Linhua</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Spectroscopic Survey of Faint Quasars in the SDSS Deep Stripe. I. Preliminary Results from the Co-added Catalog</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131.2788J</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">2788-2800</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;In this paper we present the first results of a deep spectroscopicsurvey of faint quasars in the Sloan Digital Sky Survey (SDSS) SouthernSurvey, a deep survey carried out by repeatedly imaging a 270deg&lt;sup&gt;2&lt;/sup&gt; area. Quasar candidates were selected from the deep datawith good completeness over 02, contains 414 quasars, and&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0602569</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, Rodger I.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Dickinson, Mark</style></author><author><style face="normal" font="default" size="100%">Illingworth, Garth</style></author><author><style face="normal" font="default" size="100%">Kennicutt, Robert C., Jr.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Star Formation History of the Hubble Ultra Deep Field: Comparison with the Hubble Deep Field-North</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...647..787T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">647</style></volume><pages><style face="normal" font="default" size="100%">787-798</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We use the NICMOS Treasury and ACS HUDF images to measure theextinction-corrected star formation history for 4681 galaxies in theregion common to both images using the star formation rate distributionfunction and other techniques similar to those employed with the NICMOSand WFPC2 images in the HDFN. Unlike the HDFN, the NICMOS region of theHUDF appears to lack highly luminous and high star formation rategalaxies at redshifts beyond 3. The HUDF provides a region that iscompletely uncorrelated to the HDFN and therefore provides anindependent measure of the star formation history of the universe. Thecombined HUDF and HDFN star formation rates show an average rate of 0.2M&lt;sub&gt;solar&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. The average SFR ofthe combined fields at z=1-3 is 0.29 M&lt;sub&gt;solar&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;, while the average at z=4-6 is 1.2 M&lt;sub&gt;solar&lt;/sub&gt;yr&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. The SFRs at all redshifts are within 3σ of the average over all redshifts.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0605060</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Masjedi, Morad</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Bell, Eric F.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Warren, Michael S.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Very Small Scale Clustering and Merger Rate of Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006ApJ...644...54M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">644</style></volume><pages><style face="normal" font="default" size="100%">54-60</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the small-scale (0.01 Mpc-1 Mpc)projected correlation function w&lt;sub&gt;p&lt;/sub&gt;(r&lt;sub&gt;p&lt;/sub&gt;) andreal-space correlation function ξ(r) of 24,520 luminous early-typegalaxies from the Sloan Digital Sky Survey (SDSS) Luminous Red Galaxy(LRG) sample (0.16-2 power law over more than 4 orders of magnitudein separation r. This result is too steep at small scales to beexplained in current versions of the halo model for galaxy clustering.We infer an LRG-LRG merger rate of &amp;lt;~0.6×10&lt;sup&gt;4&lt;/sup&gt;Gyr&lt;sup&gt;-1&lt;/sup&gt; Gpc&lt;sup&gt;-3&lt;/sup&gt; for this sample. This result suggeststhat the LRG-LRG mergers are not the main mode of mass growth for LRGsat z&amp;lt;0.36.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0512166</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Kilic, Mukremin</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Williams, Kurtis A.</style></author><author><style face="normal" font="default" size="100%">von Hippel, Ted</style></author><author><style face="normal" font="default" size="100%">Levine, Stephen E.</style></author><author><style face="normal" font="default" size="100%">Monet, David G.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Metcalfe, T. S.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Winget, D. E.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The White Dwarf Luminosity Function from Sloan Digital Sky Survey Imaging Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2006</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2006</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2006AJ....131..571H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">131</style></volume><pages><style face="normal" font="default" size="100%">571-581</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;A sample of white dwarfs is selected from the Sloan Digital Sky Survey(SDSS) Data Release 3 using their reduced proper motions, based onimproved proper motions from combined SDSS and USNO-B data. NumerousSDSS and follow-up spectra (Kilic and coworkers) are used to quantifycompleteness and contamination of the sample; kinematics models are usedto understand and correct for velocity-dependent selection biases. Aluminosity function is constructed covering the range7bol&amp;lt;16, and its sensitivity to various assumptionsand selection limits is discussed. The white dwarf luminosity functionbased on 6000 stars is remarkably smooth and rises nearly monotonicallyto M&lt;sub&gt;bol&lt;/sub&gt;=15.3. It then drops abruptly, although the smallnumber of low-luminosity stars in the sample and their unknownatmospheric composition prevent quantitative conclusions about thisdecline. Stars are identified that may have high tangential velocities,and a preliminary luminosity function is constructed for them.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0510820</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Baryonic Acoustic Oscillations in Simulated Galaxy Redshift Surveys</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...633..575S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">633</style></volume><pages><style face="normal" font="default" size="100%">575-588</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Baryonic acoustic oscillations imprinted in the galaxy power spectrumprovide a promising tool for probing the cosmological distance scale anddark energy. We present results from a suite of cosmological N-bodysimulations aimed at investigating possible systematic errors in therecovery of cosmological distances. We show the robustness of baryonicpeaks against nonlinearity, redshift distortions, and mild biases withinthe linear and quasi-linear regime at various redshifts. While mildlybiased tracers follow the matter power spectrum well, redshiftdistortions do partially obscure baryonic features in redshift spacecompared to real space. We calculate the statistical constraints oncosmological distortions from N-body results and compare these to theanalytic results from a Fisher matrix formalism. We conclude that theangular diameter distance will be constrained as well as in our previousFisher matrix calculations while the Hubble parameter will be lessconstrained because of nonlinear redshift distortions.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0507338</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Bridges, Terry</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jonathan</style></author><author><style face="normal" font="default" size="100%">Cannon, Russell</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Croom, Scott M.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Drinkwater, Michael</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Hewett, Paul C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Pimbblet, Kevin A.</style></author><author><style face="normal" font="default" size="100%">de Propris, Roberto</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Shanks, Tom</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Wake, David</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Calibrating photometric redshifts of luminous red galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005MNRAS.359..237P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">359</style></volume><pages><style face="normal" font="default" size="100%">237-250</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We discuss the construction of a photometric redshift catalogue ofluminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS),emphasizing the principal steps necessary for constructing such acatalogue: (i) photometrically selecting the sample, (ii) measuringphotometric redshifts and their error distributions, and (iii)estimating the true redshift distribution. We compare two photometricredshift algorithms for these data and find that they give comparableresults. Calibrating against the SDSS and SDSS-2dF (Two Degree Field)spectroscopic surveys, we find that the photometric redshift accuracy isσ~ 0.03 for redshifts less than 0.55 and worsens at higherredshift (~0.06 for z &amp;lt; 0.7). These errors are caused by photometricscatter, as well as systematic errors in the templates, filter curvesand photometric zero-points. We also parametrize the photometricredshift error distribution with a sum of Gaussians and use this modelto deconvolve the errors from the measured photometric redshiftdistribution to estimate the true redshift distribution. We pay specialattention to the stability of this deconvolution, regularizing themethod with a prior on the smoothness of the true redshift distribution.The methods that we develop are applicable to general photometricredshift surveys.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0407594</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Cosmic Homogeneity Demonstrated with Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...624...54H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">624</style></volume><pages><style face="normal" font="default" size="100%">54-58</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We test the homogeneity of the universe at z~0.3 with the luminous redgalaxy (LRG) spectroscopic sample of the Sloan Digital Sky Survey.First, the mean number N(R) of LRGs within completely surveyedLRG-centered spheres of comoving radius R is shown to be proportional toR&lt;sup&gt;3&lt;/sup&gt; at radii greater than R~70h&lt;sup&gt;-1&lt;/sup&gt;Mpc. The test hasthe virtue that it does not rely on the assumption that the LRG samplehas a finite mean density; its results show, however, that there is sucha mean density. Second, the survey sky area is divided into 10 disjointsolid angular regions, and the fractional rms density variations of theLRG sample in the redshift range 0.27h&lt;sup&gt;-3&lt;/sup&gt;Mpc&lt;sup&gt;3&lt;/sup&gt;) regions is found&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0411197</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Zhan, Hu</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Covariance of the one-dimensional mass power spectrum</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005MNRAS.357.1387Z</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">357</style></volume><pages><style face="normal" font="default" size="100%">1387-1398</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We analyse the covariance of the one-dimensional mass power spectrumalong lines of sight. The covariance reveals the correlation betweendifferent modes of fluctuations in the cosmic density field and givesthe sample variance error for measurements of the mass power spectrum.For Gaussian random fields, the covariance matrix is diagonal. Asexpected, the variance of the measured one-dimensional mass powerspectrum is inversely proportional to the number of lines of sight thatare sampled from each random field. The correlation between lines ofsight in a single field may alter the covariance. However, lines ofsight that are sampled far apart are only weakly correlated, so thatthey can be treated as independent samples. Using N-body simulations, wefind that the covariance matrix of the one-dimensional mass powerspectrum is not diagonal for the cosmic density field due to thenon-Gaussianity and that the variance is much higher than that ofGaussian random fields. From the covariance, one will be able todetermine the cosmic variance in the measured one-dimensional mass powerspectrum as well as to estimate how many lines of sight are needed toachieve a target precision.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0412632</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Dark energy and cosmic sound [review article]</style></title><secondary-title><style face="normal" font="default" size="100%">New Astronomy Reviews</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005NewAR..49..360E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">49</style></volume><pages><style face="normal" font="default" size="100%">360-365</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;I describe how acoustic oscillations imprinted into the late-timecorrelations of galaxies by baryonic physics at the epoch ofrecombination can be used as a cosmological standard ruler. Measurementsof this length scale by large galaxy surveys would allow us to computethe angular diameter distance to and Hubble parameter at the redshiftsof the survey. This in turn offers a robust way to measure theacceleration of the universe. I briefly present calculations of thestatistical performance from baseline surveys; full details of themethods and results are available in Seo and Eisenstein [ApJ, 598 (2003)720]. I discuss the advantages and disadvantages of the acousticoscillation method relative to other dark energy probes.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1016/j.newar.2005.08.005</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Borra, E. F.</style></author><author><style face="normal" font="default" size="100%">Seddiki, O.</style></author><author><style face="normal" font="default" size="100%">Angel, J. R. P.</style></author><author><style face="normal" font="default" size="100%">Worden, S. P.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Silvanandam, S.</style></author><author><style face="normal" font="default" size="100%">Hickson, P.</style></author><author><style face="normal" font="default" size="100%">Ma, K.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Deep-Field Infrared Observatory Near the Lunar Pole</style></title><secondary-title><style face="normal" font="default" size="100%">Journal of the Royal Astronomical Society of Canada</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005JRASC..99R.134B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">99</style></volume><pages><style face="normal" font="default" size="100%">134</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;A study has been made of the feasibility and scientific potential of a20-to 100-m aperture astronomical telescope at the lunar pole, with itsprimary mirror made of spinning liquid at &amp;lt; 100 K. Such a telescope,equipped with imaging and multiplexed spectroscopic instruments for adeep-infrared survey, would be revolutionary in its power to study thedistant Universe, including the formation of the first stars and theirassembly into galaxies. Our study explored the scientific opportunities,key technologies, and optimum location of such a Lunar Liquid MirrorTelescope (LLMT). An optical design for a 20- m telescope withdiffraction limited imaging over a 15-arcminute field has beendeveloped. It would be used to follow up on discoveries made with the6-m James Webb Space Telescope, with more detailed images andspectroscopic studies, as well as to detect objects 100 times fainter,such as the first high-redshift star in the early Universe. Amodel wasmade of a liquid mirror spinning on a superconducting bearing, as willbe needed for the cryogenic, vacuum environment of the LLMT. Reflectivesilver coatings have been deposited for the first time on a liquidsurface, needed to make infrared mirrors at ~80 K. Issues relating topolar locations have been explored. Dust on the optics or in a thinatmosphere, though unlikely to be problematic at the poles, should beinvestigated in-situ. Issues relating to polar locations have beenexplored. Locations at or within a few km of a pole are preferred fordeep-sky cover, and allow for long integration times by simpleinstrument rotation. This revolutionary mission concept could provide ascientific focus to NASA's planned exploration of the Moon, just ascurrently HST stands as a major achievement of its Shuttle Program.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Zheng, Zheng</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, Jim</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory</style></author><author><style face="normal" font="default" size="100%">Ivezić, Zeljko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Loh, Yeong-Shang</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffery A.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazuhiro</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...633..560E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">633</style></volume><pages><style face="normal" font="default" size="100%">560-574</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the large-scale correlation function measured from aspectroscopic sample of 46,748 luminous red galaxies from the SloanDigital Sky Survey. The survey region covers 0.72 h&lt;sup&gt;-3&lt;/sup&gt;Gpc&lt;sup&gt;3&lt;/sup&gt; over 3816 deg&lt;sup&gt;2&lt;/sup&gt; and 0.16-1 Mpcseparation that is an excellent match to the predicted shape andlocation of the imprint of the recombination-epoch acoustic oscillationson the low-redshift clustering of matter. This detection demonstratesthe linear growth of structure by gravitational instability betweenz~1000 and the present and confirms a firm prediction of the standardcosmological theory. The acoustic peak provides a standard ruler bywhich we can measure the ratio of the distances to z=0.35 and z=1089 to&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0501171</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter Rix</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Zheng, Wei</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Discovery of a Fifth Image of the Large Separation Gravitationally Lensed Quasar SDSS J1004+4112</style></title><secondary-title><style face="normal" font="default" size="100%">Publications of the Astronomical Society of Japan</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005PASJ...57L...7I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">57</style></volume><pages><style face="normal" font="default" size="100%">L7-L10</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report on the discovery of a fifth lensed image in the largeseparation lensed quasar system SDSS J1004 + 4112. A faint point sourcelocated 0.''2 from the center of the brightest galaxy in the lensingcluster was detected in images taken with the Advanced Camera forSurveys (ACS) and the Near Infrared Camera and Multi-Object Spectrometer(NICMOS) on the Hubble Space Telescope. The flux ratio between the pointsource and the brightest lensed component in the ACS image is similar tothat in the NICMOS image. The location and brightness of the pointsource are consistent with lens model predictions for a lensed image. Wetherefore conclude that the point source is likely to be a fifth lensedimage of the source quasar. In addition, the NICMOS image reveals thelensed host galaxy of the source quasar, which can strongly constrainthe structure of the lensing critical curves, and thereby the massdistribution of the lensing cluster.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0503310</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kepler, S. O.</style></author><author><style face="normal" font="default" size="100%">Castanheira, B. G.</style></author><author><style face="normal" font="default" size="100%">Saraiva, M. F. O.</style></author><author><style face="normal" font="default" size="100%">Nitta, A.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Mullally, F.</style></author><author><style face="normal" font="default" size="100%">Winget, D. E.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Discovery of fourteen new ZZ Cetis with SOAR</style></title><secondary-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005A%26A...442..629K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">442</style></volume><pages><style face="normal" font="default" size="100%">629-634</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of fourteen new ZZ Cetis with the 4.1 m SouthernAstrophysical Research telescope, at Cerro Pachon, in Chile. Thecandidates were selected from the SDSS (Sloan Digital Sky Survey) DAwhite dwarf stars with T&lt;sub&gt;eff&lt;/sub&gt; obtained from the optical spectrafit, inside the ZZ Ceti instability strip. Considering these stars aremulti-periodic pulsators and the pulsations propagate to the nucleus ofthe star, they carry information on the structure of the star andevolution of the progenitors. The ZZ Cetis discovered till 2003 aremainly within 100 pc from the Sun, and probe only the solar vicinity.The recently discovered ones, and those reported here, may sample adistinct population as they were selected mainly perpendicular to thegalactic disk and cover a distance up to ≈ 400 pc.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0507490</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Mullally, F.</style></author><author><style face="normal" font="default" size="100%">Thompson, S. E.</style></author><author><style face="normal" font="default" size="100%">Castanheira, B. G.</style></author><author><style face="normal" font="default" size="100%">Winget, D. E.</style></author><author><style face="normal" font="default" size="100%">Kepler, S. O.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Eleven New DA White Dwarf Variable Stars from the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...625..966M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">625</style></volume><pages><style face="normal" font="default" size="100%">966-972</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of 11 new variable DA white dwarf (ZZ Ceti)stars. Candidates were selected by deriving temperatures from model fitsto spectra obtained from the Sloan Digital Sky Survey (SDSS). We alsofind objects whose temperatures and gravities indicate they lie withinthe instability strip for pulsation but were not observed to vary.Although the temperatures are based on relatively low signal-to-noiseratio spectra, an impure strip is unexpected, which if confirmed, hasimplications for DA asteroseismology. This work brings the total numberof published variable DA white dwarf stars to 82.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1086/429885</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Intermediate-Scale Clustering of Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...621...22Z</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">621</style></volume><pages><style face="normal" font="default" size="100%">22-31</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the intermediate-scale (0.3-40 h&lt;sup&gt;-1&lt;/sup&gt; Mpc) clusteringof 35,000 luminous early-type galaxies at redshifts 0.16-0.44 from theSloan Digital Sky Survey. We present the redshift space two-pointcorrelation function ξ(s), the projected correlation functionw&lt;sub&gt;p&lt;/sub&gt;(r&lt;sub&gt;p&lt;/sub&gt;), and the deprojected real space correlationfunction ξ(r), for approximately volume-limited samples. As expected,the galaxies are highly clustered, with the correlation length varyingfrom 9.8+/-0.2 to 11.2 +/- 0.2 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, dependent on thespecific luminosity range. For the -23.2g&amp;lt;-21.2sample, the inferred bias relative to that of L&lt;sub&gt;*&lt;/sub&gt; galaxies is1.84+/-0.11 for1h&lt;sup&gt;-1&lt;/sup&gt;Mpcp&amp;lt;~10h&lt;sup&gt;-1&lt;/sup&gt;Mpc, with yetstronger clustering on smaller scales. We detect luminosity-dependentbias within the sample but see no evidence for redshift evolutionbetween z=0.2 and z=0.4. We find a clear indication for deviations froma power-law in the real space correlation function, with a dip at ~2h&lt;sup&gt;-1&lt;/sup&gt; Mpc scales and an upturn on smaller scales. The precisionmeasurements of these clustering trends offer new avenues for the studyof the formation and evolution of these massive galaxies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0411557</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Berlind, Andreas A.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Davé, Romeel</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Katz, Neal</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Interpreting the Relationship between Galaxy Luminosity, Color, and Environment</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...629..625B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">629</style></volume><pages><style face="normal" font="default" size="100%">625-632</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We study the relationship between galaxy luminosity, color, andenvironment in a cosmological simulation of galaxy formation. Using asimple prescription to assign colors and luminosities to simulatedgalaxies, we compare the predicted relationship with that observed forSDSS galaxies and find that the model successfully predicts most of thequalitative features seen in the data, but also shows some interestingdifferences. Specifically, the simulation predicts that the localdensity around bright red galaxies is a strong increasing function ofluminosity, but does not depend much on color at fixed luminosity.Moreover, we show that these trends are due to central galaxies in darkmatter halos whose baryonic masses correlate strongly with halo mass.The simulation also predicts that the local density around blue galaxiesis a strong increasing function of color, but does not depend much onluminosity at fixed color. We show that these trends are due tosatellite galaxies in halos whose stellar ages correlate with halo mass.Finally, the simulation fails to predict the luminosity dependence ofenvironments observed around low-luminosity red galaxies. However, weshow that this is most likely due to the simulation's limitedresolution. A study of a higher resolution, smaller volume simulationsuggests that this dependence is caused by the fact that alllow-luminosity red galaxies are satellites in massive halos, whereasintermediate-luminosity red galaxies are a mixture of satellites inmassive halos, and central galaxies in less massive halos.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0406633</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Zhan, Hu</style></author><author><style face="normal" font="default" size="100%">Davé, Romeel</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Katz, Neal</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Lyα flux power spectrum and its covariance</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005MNRAS.363.1145Z</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">363</style></volume><pages><style face="normal" font="default" size="100%">1145-1154</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We analyse the flux power spectrum and its covariance using simulatedLyα forests. We find that pseudo-hydro techniques are goodapproximations of hydrodynamical simulations at high redshift. However,the pseudo-hydro techniques fail at low redshift because they areinsufficient for characterizing some components of the low-redshiftintergalactic medium, notably the warm-hot intergalactic medium. Hence,to use the low-redshift Lyα flux power spectrum to constraincosmology, one would need realistic hydrodynamical simulations. Bycomparing (one-dimensional) mass statistics with flux statistics, weshow that the non-linear transform between density and flux quenches thefluctuations so that the flux power spectrum is much less sensitive tocosmological parameters than the one-dimensional mass power spectrum.The covariance of the flux power spectrum is nearly Gaussian. As such,the uncertainties of the underlying mass power spectrum could still belarge, even though the flux power spectrum can be precisely determinedfrom a small number of lines of sight.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0504419</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Vanlandingham, Karen M.</style></author><author><style face="normal" font="default" size="100%">Schmidt, Gary D.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Stinson, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Wolfe, Michael A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Magnetic White Dwarfs from the SDSS. II. The Second and Third Data Releases</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005AJ....130..734V</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">130</style></volume><pages><style face="normal" font="default" size="100%">734-741</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Fifty-two magnetic white dwarfs have been identified in spectroscopicobservations from the Sloan Digital Sky Survey (SDSS) obtained betweenmid-2002 and the end of 2004, including Data Releases 2 and 3. Althoughnot as numerous or diverse as the discoveries from the first datarelease, the collection exhibits polar field strengths ranging from 1.5to ~1000 MG and includes two new unusual atomic DQA examples, amolecular DQ, and five stars that show hydrogen in fields above 500 MG.The highest field example, SDSS J2346+3853, may be the most stronglymagnetic white dwarf yet discovered. Analysis of the photometric dataindicates that the magnetic sample spans the same temperature range asfor nonmagnetic white dwarfs from the SDSS, and support is found forprevious claims that magnetic white dwarfs tend to have larger massesthan their nonmagnetic counterparts. A glaring exception to this trendis the apparently low-gravity object SDSS J0933+1022, which may have ahistory involving a close binary companion.A portion of the results presented here were obtained with the MMTObservatory, a facility operated jointly by the University of Arizonaand the Smithsonian Institution.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0505085</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Stern, Daniel</style></author><author><style face="normal" font="default" size="100%">Eisenhardt, Peter</style></author><author><style face="normal" font="default" size="100%">Gorjian, Varoujan</style></author><author><style face="normal" font="default" size="100%">Kochanek, Christopher S.</style></author><author><style face="normal" font="default" size="100%">Caldwell, Nelson</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Brodwin, Mark</style></author><author><style face="normal" font="default" size="100%">Brown, Michael J. I.</style></author><author><style face="normal" font="default" size="100%">Cool, Richard</style></author><author><style face="normal" font="default" size="100%">Dey, Arjun</style></author><author><style face="normal" font="default" size="100%">Green, Paul</style></author><author><style face="normal" font="default" size="100%">Jannuzi, Buell T.</style></author><author><style face="normal" font="default" size="100%">Murray, Stephen S.</style></author><author><style face="normal" font="default" size="100%">Pahre, Michael A.</style></author><author><style face="normal" font="default" size="100%">Willner, S. P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Mid-Infrared Selection of Active Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...631..163S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">631</style></volume><pages><style face="normal" font="default" size="100%">163-168</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Mid-infrared photometry provides a robust technique for identifyingactive galaxies. While the ultraviolet to mid-infrared (λ&amp;lt;~5μm) continuum of stellar populations is dominated by the compositeblackbody curve and peaks at approximately 1.6 μm, the ultraviolet tomid-infrared continuum of active galactic nuclei (AGNs) is dominated bya power law. Consequently, with a sufficient wavelength baseline, onecan easily distinguish AGNs from stellar populations. Mirroring thetendency of AGNs to be bluer than galaxies in the ultraviolet, wheregalaxies (and stars) sample the blue, rising portion of stellar spectra,AGNs tend to be redder than galaxies in the mid-infrared, where galaxiessample the red, falling portion of the stellar spectra. We report onSpitzer Space Telescope mid-infrared colors, derived from the IRACShallow Survey, of nearly 10,000 spectroscopically identified sourcesfrom the AGN and Galaxy Evolution Survey. On the basis of thisspectroscopic sample, we find that simple mid-infrared color criteriaprovide remarkably robust separation of active galaxies from normal&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0410523</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Thompson, Rodger I.</style></author><author><style face="normal" font="default" size="100%">Illingworth, Garth</style></author><author><style face="normal" font="default" size="100%">Bouwens, Rychard</style></author><author><style face="normal" font="default" size="100%">Dickinson, Mark</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Franx, Marijn</style></author><author><style face="normal" font="default" size="100%">Riess, Adam</style></author><author><style face="normal" font="default" size="100%">Rieke, Marcia J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Glenn</style></author><author><style face="normal" font="default" size="100%">Stobie, Elizabeth</style></author><author><style face="normal" font="default" size="100%">Toft, Sune</style></author><author><style face="normal" font="default" size="100%">van Dokkum, Pieter</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Near-Infrared Camera and Multi-Object Spectrometer Ultra Deep Field: Observations, Data Reduction, and Galaxy Photometry</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005AJ....130....1T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">130</style></volume><pages><style face="normal" font="default" size="100%">1-12</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper describes the observations and data reduction techniques forthe version 2.0 images and catalog of the Near-Infrared Camera andMulti-Object Spectrometer Ultra Deep Field (NICMOS UDF) Treasuryprogram. All sources discussed in this paper are based on detections inthe combined NICMOS F110W and F160W bands only. The NICMOS images aredrizzled to 0.09&quot; pixel&lt;sup&gt;-1&lt;/sup&gt; and aligned to the Advanced Camerafor Surveys UDF F850LP image, which was rebinned to the same pixelscale. These form the NICMOS version 2.0 UDF images. The catalog sourcesare chosen with a conservative detection limit to avoid the inclusion ofnumerous spurious sources. The catalog contains 1293 objects in the144&lt;sup&gt;''&lt;/sup&gt;×144&lt;sup&gt;''&lt;/sup&gt; NICMOS subfield of the UDF. The5 σ signal-to-noise ratio level is an average 0.6&quot; diameteraperture AB magnitude of 27.7 at 1.1 and 1.6 μm. The catalog sources,listed in order of right ascension, satisfy a minimum signal-to-noiseratio criterion of 1.4 σ in at least seven contiguous pixels ofthe combined F110W and F160W image.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0503504</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...629..143B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">629</style></volume><pages><style face="normal" font="default" size="100%">143-157</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We examine the relationship between environment and the luminosities,surface brightnesses, colors, and profile shapes of luminous galaxies inthe Sloan Digital Sky Survey (SDSS). For the SDSS sample, galaxy coloris the galaxy property most predictive of the local environment. Galaxycolor and luminosity-measures of the star formation history-jointlycomprise the most predictive pair of properties. At fixed luminosity andcolor, density is not closely related to surface brightness or toSérsic index-measures of galaxy structure. In the text, wediscuss what measurable residual relationships exist, generally findingthat at red colors and fixed luminosity, the mean density decreases atthe highest surface brightnesses and Sérsic indices. In general,these results suggest that the structural properties of galaxies areless closely related to galaxy environment than are their masses andstar formation histories.Based on observations obtained with the Sloan Digital Sky Survey.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0310453</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Schechter, Paul L.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">White, Richard L.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J024634.11-082536.2: A New Gravitationally Lensed Quasar from the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005AJ....130.1967I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">130</style></volume><pages><style face="normal" font="default" size="100%">1967-1976</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of a new two-image gravitationally lensedquasar, SDSS J024634.11-082536.2 (SDSS J0246-0825). This object wasselected as a lensed quasar candidate from the Sloan Digital Sky Survey(SDSS) by the same algorithm that was used to discover other SDSS lensedquasars (e.g., SDSS J0924+0219). Multicolor imaging with the MagellanConsortium's Walter Baade 6.5 m telescope and spectroscopic observationsusing the W. M. Keck Observatory's Keck II telescope confirm that SDSSJ0246-0825 consists of two lensed images (Δθ=1.04&quot;) of asource quasar at z=1.68. Imaging observations with the Keck I telescopeand the Hubble Space Telescope reveal an extended object between the twoquasar components, which is likely to be a lensing galaxy of thissystem. From the absorption lines in the spectra of the quasarcomponents and the apparent magnitude of the galaxy, combined with theexpected absolute magnitude from the Faber-Jackson relation, we estimatethe redshift of the lensing galaxy to be z=0.724. A highly distortedring is visible in the Hubble Space Telescope images, which is likely tobe the lensed host galaxy of the source quasar. Simple mass modelingpredicts the possibility that there is a small (faint) lensing objectnear the primary lensing galaxy.Based on observations with the NASA/ESA Hubble Space Telescope, obtainedat the Space Telescope Science Institute, which is operated by theAssociation of Universities for Research in Astronomy (AURA), Inc.,under NASA contract NAS5-26555. These observations are associated withHST program 9744.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0506631</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Barentine, J. C.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Saxe, David H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey Quasar Catalog. III. Third Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005AJ....130..367S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">130</style></volume><pages><style face="normal" font="default" size="100%">367-380</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the third edition of the Sloan Digital Sky Survey (SDSS)Quasar Catalog. The catalog consists of the 46,420 objects in the SDSSThird Data Release that have luminosities larger than M&lt;sub&gt;i&lt;/sub&gt;=-22(in a cosmology with H&lt;sub&gt;0&lt;/sub&gt;=70 km s&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-1&lt;/sup&gt;, Ω&lt;sub&gt;M&lt;/sub&gt;=0.3, andΩ&lt;sub&gt;Λ&lt;/sub&gt;=0.7), have at least one emission line withFWHM larger than 1000 km s&lt;sup&gt;-1&lt;/sup&gt; or are unambiguously broadabsorption line quasars, are fainter than i=15.0, and have highlyreliable redshifts. The area covered by the catalog is ~4188deg&lt;sup&gt;2&lt;/sup&gt;. The quasar redshifts range from 0.08 to 5.41, with amedian value of 1.47; the high-redshift sample includes 520 quasars atredshifts greater than 4, of which 17 are at redshifts greater than 5.For each object the catalog presents positions accurate to better than0.2&quot; rms per coordinate, five-band (ugriz) CCD-based photometry withtypical accuracy of 0.03 mag, and information on the morphology andselection method. The catalog also contains radio, near-infrared, andX-ray emission properties of the quasars, when available, from otherlarge-area surveys. The calibrated digital spectra cover the wavelengthregion 3800-9200 Å at a spectral resolution of ~=2000 the spectracan be retrieved from the public database using the information providedin the catalog. A total of 44,221 objects in the catalog were discoveredby the SDSS; 28,400 of the SDSS discoveries are reported here for thefirst time.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0503679</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Baldry, I. K.</style></author><author><style face="normal" font="default" size="100%">Glazebrook, K.</style></author><author><style face="normal" font="default" size="100%">Budavári, T.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Annis, J.</style></author><author><style face="normal" font="default" size="100%">Bahcall, N. A.</style></author><author><style face="normal" font="default" size="100%">Blanton, M. R.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Csabai, I.</style></author><author><style face="normal" font="default" size="100%">Heckman, T. M.</style></author><author><style face="normal" font="default" size="100%">H Lin</style></author><author><style face="normal" font="default" size="100%">Loveday, J.</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Schneider, D. P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey u-band Galaxy Survey: luminosity functions and evolution</style></title><secondary-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005MNRAS.358..441B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">358</style></volume><pages><style face="normal" font="default" size="100%">441-456</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We construct and analyse a u-band selected galaxy sample from the SloanDigital Sky Survey (SDSS) Southern Survey, which covers275deg&lt;sup&gt;2&lt;/sup&gt;. The sample includes 43223 galaxies withspectroscopic redshifts in the range 0.005 &amp;lt; z &amp;lt; 0.3 and with 14.5&amp;lt; u &amp;lt; 20.5. The signal-to-noise (S/N) ratio in the u-bandPetrosian aperture is improved by co-adding multiple epochs of imagingdata and by including sky-subtraction corrections. Luminosity functionsfor the near-UV &lt;sup&gt;0.1&lt;/sup&gt;u band (λ~ 322 +/- 26nm) aredetermined in redshift slices of width 0.02, which show a highlysignificant evolution in M* of -0.8 +/- 0.1 mag between z= 0 and 0.3;with M*-5 logh&lt;sub&gt;70&lt;/sub&gt;=-18.84 +/- 0.05 (AB mag), logφ*=-2.06+/- 0.03 (h&lt;sup&gt;3&lt;/sup&gt;&lt;sub&gt;70&lt;/sub&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;) andlogρ&lt;sub&gt;L&lt;/sub&gt;= 19.11 +/- 0.02(h&lt;sub&gt;70&lt;/sub&gt;WHz&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;) at z= 0.1. Thefaint-end slope determined for z &amp;lt; 0.06 is given by α=-1.05 +/-0.08. This is in agreement with recent determinations from the GalaxyEvolution Explorer at shorter wavelengths. Comparing our z &amp;lt; 0.3luminosity density measurements with 0.2 &amp;lt; z &amp;lt; 1.2 fromClassifying Objects by Medium Band Observations in 17 Filters(COMBO-17), we find that the 280-nm density evolves asρ&lt;sub&gt;L&lt;/sub&gt;~ (1 +z)&lt;sup&gt;β&lt;/sup&gt; with β= 2.1 +/- 0.2; andfind no evidence for any change in slope over this redshift range. Bycomparing with other measurements of cosmic star formation history, weestimate that the effective dust attenuation at 280nm has increased by0.8 +/- 0.3mag between z= 0 and 1.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0501110</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Schneider, Don</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Small-Scale Clustering of Luminous Red Galaxies via Cross-Correlation Techniques</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005ApJ...619..178E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">619</style></volume><pages><style face="normal" font="default" size="100%">178-192</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the small-scale (0.2-7 h&lt;sup&gt;-1&lt;/sup&gt; Mpc) cross-correlationsbetween 32,000 luminous early-type galaxies and a reference sample of 16million normal galaxies from the Sloan Digital Sky Survey (SDSS). Ourmethod allows us to construct the spherically averaged, real-spacecross-correlation function between the spectroscopic luminous red galaxy(LRG) sample and galaxies from the SDSS imaging. We report thecross-correlation as a function of scale, luminosity, and redshift. Wefind very strong luminosity dependences in the clustering amplitudes, upto a factor of 4 over a factor of 4 in luminosity, and we measure thisdependence with a high signal-to-noise ratio. The luminosity dependenceof bias is found to depend on scale, with more variation on smallerscales. The clustering as a function of scale is not a power law butinstead has a dip at 1 h&lt;sup&gt;-1&lt;/sup&gt; Mpc and an excess on small scales.The fraction of red galaxies within the L&lt;sup&gt;*&lt;/sup&gt; sample surroundingLRGs is a strong function of scale, as expected. However, the fractionof red galaxies evolves in redshift similarly on small and large scales,suggesting that cluster and field populations are changing in the samemanner. The results highlight the advantage on small scales of usingcross-correlation methods as a means of avoiding shot noise in samplesof rare galaxies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0411559</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Abazajian, Kevork</style></author><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Anderson, Kurt S. J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Bastian, Steven</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J., Jr.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard J.</style></author><author><style face="normal" font="default" size="100%">Briggs, John W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carey, Larry N.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Covey, Kevin R.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Dalcanton, Julianne J.</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Dong, Feng</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Gurbani, Vijay K.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Hamabe, Masaru</style></author><author><style face="normal" font="default" size="100%">Harbeck, Daniel</style></author><author><style face="normal" font="default" size="100%">Harris, Frederick H.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Hayes, Jeffrey</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hogan, Craig J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holmgren, Donald J.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Takashi</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kniazev, Alexei Yu.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Mannery, Ed</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Martínez-Delgado, David</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Ménard, Brice</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nash, Thomas</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">O'Mullane, William</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Pauls, George</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Pourbaix, Dimitri</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas R.</style></author><author><style face="normal" font="default" size="100%">Raddick, M. Jordan</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schroeder, Joshua</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sekiguchi, Maki</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Szokoly, Gyula P.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Teodoro, Luis</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Walkowicz, Lucianne M.</style></author><author><style face="normal" font="default" size="100%">Wang, Shu-i.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilhite, Brian C.</style></author><author><style face="normal" font="default" size="100%">Xu, Yongzhong</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yasuda, Naoki</style></author><author><style face="normal" font="default" size="100%">Yip, Ching-Wa</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zibetti, Stefano</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Third Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2005</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2005</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2005AJ....129.1755A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">129</style></volume><pages><style face="normal" font="default" size="100%">1755-1759</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;This paper describes the Third Data Release of the Sloan Digital SkySurvey (SDSS). This release, containing data taken up through 2003 June,includes imaging data in five bands over 5282 deg&lt;sup&gt;2&lt;/sup&gt;,photometric and astrometric catalogs of the 141 million objects detectedin these imaging data, and spectra of 528,640 objects selected over 4188deg&lt;sup&gt;2&lt;/sup&gt;. The pipelines analyzing both images and spectroscopyare unchanged from those used in our Second Data Release.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0410239</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Dahn, Conard C.</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Schmidt, Gary</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Collinge, Matthew J.</style></author><author><style face="normal" font="default" size="100%">Mukadam, A. S.</style></author><author><style face="normal" font="default" size="100%">Koester, D.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Schlegel, D. J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Lamb, D. Q.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Catalog of Spectroscopically Identified White Dwarf Stars in the First Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...607..426K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">607</style></volume><pages><style face="normal" font="default" size="100%">426-444</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the full spectroscopic white dwarf and hot subdwarf samplefrom the Sloan Digital Sky Survey (SDSS) first data release, DR1. Wefind 2551 white dwarf stars of various types, 240 hot subdwarf stars,and an additional 144 objects we have identified as uncertain whitedwarf stars. Of the white dwarf stars, 1888 are nonmagnetic DA types and171 are nonmagnetic DBs. The remaining (492) objects consist of alldifferent types of white dwarf stars: DO, DQ, DC, DH, DZ, hybrid starssuch as DAB, etc., and those with nondegenerate companions. We fit theDA and DB spectra with a grid of models to determine the T&lt;sub&gt;eff&lt;/sub&gt;and logg for each object. For all objects, we provide coordinates,proper motions, SDSS photometric magnitudes, and enough information toretrieve the spectrum/image from the SDSS public database. This catalognearly doubles the known sample of spectroscopically identified whitedwarf stars. In the DR1 imaged area of the sky, we increase the knownsample of white dwarf stars by a factor of 8.5. We also comment onseveral particularly interesting objects in this sample.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0402209</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Budavari, Tamas</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szapudi, Istvan</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">{SDSS Collaboration}</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Cosmological Parameters from Eigenmode Analysis of Sloan Digital Sky Survey Galaxy Redshifts</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">June 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...607..655P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">607</style></volume><pages><style face="normal" font="default" size="100%">655-660</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present estimates of cosmological parameters from the application ofthe Karhunen-Loève transform to the analysis of thethree-dimensional power spectrum of density fluctuations using SloanDigital Sky Survey galaxy redshifts. We use Ω&lt;sub&gt;m&lt;/sub&gt;h andf&lt;sub&gt;b&lt;/sub&gt;=Ω&lt;sub&gt;b&lt;/sub&gt;/Ω&lt;sub&gt;m&lt;/sub&gt; to describe theshape of the power spectrum, σ&lt;sup&gt;L&lt;/sup&gt;&lt;sub&gt;8g&lt;/sub&gt; for the(linearly extrapolated) normalization, and β to parameterize lineartheory redshift-space distortions. On scales k&amp;lt;~0.16hMpc&lt;sup&gt;-1&lt;/sup&gt;, our maximum likelihood values areΩ&lt;sub&gt;m&lt;/sub&gt;h=0.264+/-0.043, f&lt;sub&gt;b&lt;/sub&gt;=0.286+/-0.065,σ&lt;sup&gt;L&lt;/sup&gt;&lt;sub&gt;8g&lt;/sub&gt;=0.966+/-0.048, and β=0.45+/-0.12.When we take a prior on Ω&lt;sub&gt;b&lt;/sub&gt; from the Wilkinson MicrowaveAnisotropy Probe (WMAP), we find Ω&lt;sub&gt;m&lt;/sub&gt;h=0.207+/-0.030,which is in excellent agreement with WMAP and the Two-Degree Field. Thisindicates that we have reasonably measured the gross shape of the powerspectrum, but we have difficulty breaking the degeneracy betweenΩ&lt;sub&gt;m&lt;/sub&gt;h and f&lt;sub&gt;b&lt;/sub&gt;, because the baryon oscillationsare not resolved in the current spectroscopic survey window function.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0401249</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Abazajian, Kevork</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Sandvik, Havard</style></author><author><style face="normal" font="default" size="100%">Wang, Xiaomin</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Hoyle, Fiona</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Budavari, Tamás</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Xu, Yongzhong</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Hennessy, Greg</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Liam</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Cosmological parameters from SDSS and WMAP</style></title><secondary-title><style face="normal" font="default" size="100%">Physical Review D</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004PhRvD..69j3501T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">69</style></volume><pages><style face="normal" font="default" size="100%">103501</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We measure cosmological parameters using the three-dimensional powerspectrum P(k) from over 200 000 galaxies in the Sloan Digital Sky Survey(SDSS) in combination with Wilkinson Microwave Anisotropy Probe (WMAP)and other data. Our results are consistent with a “vanilla”flat adiabatic cold dark matter model with a cosmological constantwithout tilt (n&lt;sub&gt;s&lt;/sub&gt;=1), running tilt, tensor modes, or massiveneutrinos. Adding SDSS information more than halves the WMAP-only errorbars on some parameters, tightening 1σ constraints on the Hubbleparameter from h≈0.74&lt;sup&gt;+0.18&lt;/sup&gt;&lt;sub&gt;-0.07&lt;/sub&gt; toh≈0.70&lt;sup&gt;+0.04&lt;/sup&gt;&lt;sub&gt;-0.03&lt;/sub&gt;, on the matter density fromΩ&lt;sub&gt;m&lt;/sub&gt;≈0.25±0.10 toΩ&lt;sub&gt;m&lt;/sub&gt;≈0.30±0.04 (1σ) and on neutrino&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0310723</style></custom3><reprint-edition><style face="normal" font="default" size="100%">other sources should allow these to be substantially tightened.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Brinchmann, Jarle</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Dependence on Environment of the Color-Magnitude Relation of Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">January 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...601L..29H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">601</style></volume><pages><style face="normal" font="default" size="100%">L29-L32</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The distribution in color and absolute magnitude is presented for 55,158galaxies taken from the Sloan Digital Sky Survey in the redshift range0.08-1 Mpc and line-of-sighthalf-length 8 h&lt;sup&gt;-1&lt;/sup&gt; Mpc. In all environments, bulge-dominatedgalaxies (defined to be those with radial profiles best fitted withlarge Sérsic indices) have a color-magnitude diagram dominated byred galaxies for which the mode of the color distribution at fixedabsolute magnitude depends linearly on absolute magnitude. Although themost luminous galaxies reside preferentially in high-density regions andblue galaxies reside preferentially in low-density regions, there isonly a barely detectable variation with overdensity in the color (zeropoint) or slope of the linear relation between the mode color andluminosity [&amp;lt;0.02 mag in &lt;sup&gt;0.1&lt;/sup&gt;(g-r) or (B-V)]. These resultsconstrain variations with environmental density in the ages or&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0307336</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bouwens, R. J.</style></author><author><style face="normal" font="default" size="100%">Thompson, R. I.</style></author><author><style face="normal" font="default" size="100%">Illingworth, G. D.</style></author><author><style face="normal" font="default" size="100%">Franx, M.</style></author><author><style face="normal" font="default" size="100%">van Dokkum, P. G.</style></author><author><style face="normal" font="default" size="100%">Fan, X.</style></author><author><style face="normal" font="default" size="100%">Dickinson, M. E.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Rieke, M. J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Galaxies at z~7-8: z850-Dropouts in the Hubble Ultra Deep Field</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...616L..79B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">616</style></volume><pages><style face="normal" font="default" size="100%">L79-L82</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We have detected likely z~7-8 galaxies in the144&lt;sup&gt;''&lt;/sup&gt;×144&lt;sup&gt;''&lt;/sup&gt; Near-Infrared Camera andMulti-Object Spectrometer (NICMOS) observations of the Hubble Ultra DeepField. Objects are required to be &amp;gt;=3 σ detections in bothNICMOS bands, J&lt;sub&gt;110&lt;/sub&gt; and H&lt;sub&gt;160&lt;/sub&gt;. The selectioncriteria for this sample are(z&lt;sub&gt;850&lt;/sub&gt;-J&lt;sub&gt;110&lt;/sub&gt;)&lt;sub&gt;AB&lt;/sub&gt;&amp;gt;0.8,(z&lt;sub&gt;850&lt;/sub&gt;-J&lt;sub&gt;110&lt;/sub&gt;)&lt;sub&gt;AB&lt;/sub&gt;&amp;gt;0.66(J&lt;sub&gt;110&lt;/sub&gt;-H&lt;sub&gt;160&lt;/sub&gt;)&lt;sub&gt;AB&lt;/sub&gt;+0.8,(J&lt;sub&gt;110&lt;/sub&gt;-H&lt;sub&gt;160&lt;/sub&gt;)&lt;sub&gt;AB&lt;/sub&gt;&amp;lt;1.2 and no detectionat less than 8500 Å. The five selected sources have totalmagnitudes H&lt;sub&gt;160,AB&lt;/sub&gt;~27. Four of the five sources are quiteblue compared to typical lower redshift dropout galaxies and areclustered within a 1 arcmin&lt;sup&gt;2&lt;/sup&gt; region. Because all five sourcesare near the limit of the NICMOS data, we have carefully evaluated theirreality. Each of the candidates is visible in different splits of thedata and a median stack. We analyzed several noise images and estimatethe number of spurious sources to be 1+/-1. A search using anindependent reduction of this same data set clearly revealed three ofthe five candidates and weakly detected a fourth candidate, suggestingthat the contamination could be higher. For comparison with predictionsfrom lower redshift samples, we take a conservative approach and adoptfour z~7-8 galaxies as our sample. With the same detection criteria onsimulated data sets, assuming no evolution from z~3.8, we predict 10sources at z~7-8, or 14 if we use a more realistic (1+z)&lt;sup&gt;-1&lt;/sup&gt;size scaling. We estimate that the rest-frame continuum UV (~1800Å) luminosity density at z~7.5 (integrated down to0.3L&lt;sup&gt;*&lt;/sup&gt;&lt;sub&gt;z=3&lt;/sub&gt;) is just0.20&lt;sup&gt;+0.12&lt;/sup&gt;&lt;sub&gt;-0.08&lt;/sub&gt; times that found at z~3.8 (or0.20&lt;sup&gt;+0.23&lt;/sup&gt;&lt;sub&gt;-0.12&lt;/sub&gt; times this quantity includingcosmic variance). Effectively this sets an upper limit on the luminositydensity down to 0.3L&lt;sup&gt;*&lt;/sup&gt;&lt;sub&gt;z=3&lt;/sub&gt; and is consistent withsignificant evolution at the bright end of the luminosity function fromz~7.5 to 3.8. Even with the lower UV luminosity density at z~7.5, itappears that galaxies could still play an important role in reionizationat these redshifts, although definitive measurements remain to be made.Based on observations made with the NASA/ESA Hubble Space Telescope,which is operated by the Association of Universities for Research inAstronomy, Inc., under NASA contract NAS 5-26555.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0409488</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Bergeron, P.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Harris, H. C.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Helium White Dwarf of Extremely Low Mass</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...606L.147L</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">606</style></volume><pages><style face="normal" font="default" size="100%">L147-L149</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We analyze the spectrum of an unusually low mass white dwarf, SDSSJ123410.37-022802.9 (0335-264-52000), found in our recent, white dwarfcatalog from the first data release (DR1) of the Sloan Digital SkySurvey (SDSS). Two independent, model atmosphere fits result in anaccurate determination of atmospheric and stellar parameters. The morehands-on analysis yields T&lt;sub&gt;eff&lt;/sub&gt;=17,470+/-750 K andlogg=6.38+/-0.05. We argue that the object cannot be a main-sequence Astar, a horizontal-branch star, or a subdwarf B star. Instead, it isinterpreted as a very low mass white dwarf with a core composed ofhelium, with mass ~0.18-0.19 M&lt;sub&gt;solar&lt;/sub&gt;, similar to thatpublished previously for the unusual companion to the millisecond pulsarJ1012+5307. The star probably remains in a binary, perhaps even with anundiscovered or dead pulsar companion. However, the companion might be amore ordinary star, provided Roche lobe mass transfer began shortlyafter the now-visible component left the main sequence. A second SDSSlow-mass white dwarf candidate is also analyzed, but the spectrum forthis fainter object is of poorer quality. The sample appears to includeadditional, similar candidates, worthy of more accurate observation.Correct identification of any additional white dwarfs of extremely lowmass requires careful observation and interpretation.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0404291</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Zheng, Wei</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Suto, Yasushi</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jonathan</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Goto, Tomotsugu</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin Scott</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Observations and Theoretical Implications of the Large-Separation Lensed Quasar SDSS J1004+4112</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...605...78O</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">605</style></volume><pages><style face="normal" font="default" size="100%">78-97</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We study the recently discovered gravitational lens SDSS J1004+4112, thefirst quasar lensed by a cluster of galaxies. It consists of four imageswith a maximum separation of 14.62&quot;. The system was selected from thephotometric data of the Sloan Digital Sky Survey (SDSS) and has beenconfirmed as a lensed quasar at z=1.734 on the basis of deep imaging andspectroscopic follow-up observations. We present color-magnituderelations for galaxies near the lens plus spectroscopy of three centralcluster members, which unambiguously confirm that a cluster at z=0.68 isresponsible for the large image separation. We find a wide range of lensmodels consistent with the data, and despite considerable diversity theysuggest four general conclusions: (1) the brightest cluster galaxy andthe center of the cluster potential well appear to be offset by severalkiloparsecs; (2) the cluster mass distribution must be elongated in thenorth-south direction, which is consistent with the observeddistribution of cluster galaxies; (3) the inference of a large tidalshear (~0.2) suggests significant substructure in the cluster; and (4)enormous uncertainty in the predicted time delays between the imagesmeans that measuring the delays would greatly improve constraints on themodels. We also compute the probability of such large-separation lensingin the SDSS quasar sample on the basis of the cold dark matter model.The lack of large-separation lenses in previous surveys and thediscovery of one in SDSS together imply a mass fluctuation normalization&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0312429</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Niederste-Ostholt, Martin</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Quasar without Broad Lyα Emission</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AJ....128..534H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">128</style></volume><pages><style face="normal" font="default" size="100%">534-543</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The z=3.02 quasar SDSS J095253.83+011421.9 exhibits broad metal-lineemission (C IV FWHM~=9000 km s&lt;sup&gt;-1&lt;/sup&gt;), but broad Lyαemission is not present. Instead, only a narrow Lyα line isobserved (FWHM~=1140 km s&lt;sup&gt;-1&lt;/sup&gt;). The large CIV/Lyα ratioin the broad-line region (BLR) emission from this object can be matchedmost closely by a BLR dominated by gas at very high densities(10&lt;sup&gt;15&lt;/sup&gt; cm&lt;sup&gt;-3&lt;/sup&gt;), which suppresses the Lyαemission, and illuminated by an incident power law extending to ~200μm, which yields increased emission from purely collisionally excitedcoolant lines (such as C IV, N V, and O VI) but not from recombinationlines like Lyα. However, the strong C III emission predicted bythis model is not observed, and the observed broad C III] emission mustcome from a lower density BLR component and should be accompanied bybroad Lyα emission, which is not observed. The least unlikelyexplanation for this spectrum seems to be that any intrinsic broadLyα emission is removed by smooth N V absorption in the red wingof the Lyα emission line and by smooth Lyα absorption in theblue wing of the Lyα emission line. This postulated smoothabsorption would be in addition to the strong, associated, narrowabsorption seen in numerous ions. Smooth absorption in Lyα, N V,and O VI, but not in C IV, would be unusual, but not impossible,although it is suspicious that the postulated absorption must almostexactly cancel the postulated intrinsic broad emission. We conclude thatthe spectrum of SDSS J0952+0114 appears unique (among ~=3600 SDSSspectra of quasars at z&amp;gt;2.12) because of some combination of unusualparameters, and we discuss possible observations to determine thecombination of circumstances responsible for the spectrum.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0405239</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ivezić, Ž.</style></author><author><style face="normal" font="default" size="100%">Lupton, R. H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, D.</style></author><author><style face="normal" font="default" size="100%">Boroski, B.</style></author><author><style face="normal" font="default" size="100%">Adelman-McCarthy, J.</style></author><author><style face="normal" font="default" size="100%">Yanny, B.</style></author><author><style face="normal" font="default" size="100%">Kent, S.</style></author><author><style face="normal" font="default" size="100%">Stoughton, C.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, D.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, N.</style></author><author><style face="normal" font="default" size="100%">Rockosi, C. M.</style></author><author><style face="normal" font="default" size="100%">Gunn, J. E.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Strauss, M. A.</style></author><author><style face="normal" font="default" size="100%">Richards, G. T.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D.</style></author><author><style face="normal" font="default" size="100%">Nicinski, T.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, J.</style></author><author><style face="normal" font="default" size="100%">Newman, P. R.</style></author><author><style face="normal" font="default" size="100%">Snedden, S.</style></author><author><style face="normal" font="default" size="100%">Thakar, A. R.</style></author><author><style face="normal" font="default" size="100%">Szalay, A.</style></author><author><style face="normal" font="default" size="100%">Munn, J. A.</style></author><author><style face="normal" font="default" size="100%">Smith, J. A.</style></author><author><style face="normal" font="default" size="100%">Tucker, D.</style></author><author><style face="normal" font="default" size="100%">Lee, B.C</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS data management and photometric quality assessment</style></title><secondary-title><style face="normal" font="default" size="100%">Astronomische Nachrichten</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AN....325..583I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">325</style></volume><pages><style face="normal" font="default" size="100%">583-589</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We summarize the Sloan Digital Sky Survey data acquisition andprocessing steps, and describe runQA, a pipeline designed for automateddata quality assessment. In particular, we show how the position of thestellar locus in color-color diagrams can be used to estimate theaccuracy of photometric zeropoint calibration to better than 0.01 mag in0.03 deg&lt;sup&gt;2&lt;/sup&gt; patches. Using this method, we estimate thattypical photometric zeropoint calibration errors for SDSS imaging dataare not larger than ˜0.01 mag in the g, r, and i bands, 0.02 magin the z band, and 0.03 mag in the u band (root-mean-scatter forzeropoint offsets).&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0410195</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Pindor, Bart</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sekiguchi, Maki</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J115517.35+634622.0: A Newly Discovered Gravitationally Lensed Quasar</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AJ....127.1318P</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">127</style></volume><pages><style face="normal" font="default" size="100%">1318-1324</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of SDSS J115517.35+634622.0, a previouslyunknown gravitationally lensed quasar. The lens system exhibits twoimages of a z=2.89 quasar, with an image separation of 1.832&quot;+/-0.007&quot;.Near-IR imaging of the system reveals the presence of the lensing galaxybetween the two quasar images. Based on absorption features seen in theSloan Digital Sky Survey (SDSS) spectrum, we determine a lens galaxyredshift of z=0.1756. The lens is rather unusual in that one of thequasar images is only 0.22&quot;+/-0.07&quot; (~0.1 R&lt;sub&gt;eff&lt;/sub&gt;) from thecenter of the lens galaxy, and photometric modeling indicates that thisimage is significantly brighter than predicted by a SIS model. Thissystem was discovered in the course of an ongoing search for stronglylensed quasars in the data set from the SDSS.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0312176</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jonathan</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Schechter, Paul L.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J1335+0118: A New Two-Image Gravitational Lens</style></title><secondary-title><style face="normal" font="default" size="100%">Publications of the Astronomical Society of Japan</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004PASJ...56..399O</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">56</style></volume><pages><style face="normal" font="default" size="100%">399-405</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report on the discovery of the two-image gravitationally lensedquasar SDSSJ1335 + 0118. The object was selected as a lens candidatefrom the Sloan Digital Sky Survey. The imaging and spectroscopicfollow-up observations confirm that the system exhibits twogravitationally lensed images of a quasar at z = 1.57. The imageseparation is 1''.56. We also detect an extended component between thetwo quasar images, likely to be a lensing galaxy. Preliminary massmodeling predicts a differential time delay, Δt of ˜30h&lt;sup&gt;-1&lt;/sup&gt; day, assuming the redshift of the lens galaxy to be 0.5.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0311169</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Abazajian, Kevork</style></author><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Anderson, Kurt</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Bastian, Steven</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J., Jr.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Briggs, John W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carey, Larry N.</style></author><author><style face="normal" font="default" size="100%">Carliles, Samuel</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Dong, Feng</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gal, Roy R.</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Gurbani, Vijay K.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Hamabe, Masaru</style></author><author><style face="normal" font="default" size="100%">Harris, Frederick H.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hogan, Craig J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holmgren, Donald J.</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Takashi</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kniazev, Alexei Yu.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter Z.</style></author><author><style face="normal" font="default" size="100%">Kuropatkin, Nickolai</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Li, Nolan</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Loh, Yeong-Shang</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Malik, Tanu</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Nash, Thomas</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">O'Mullane, William</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas R.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sekiguchi, Maki</style></author><author><style face="normal" font="default" size="100%">Seljak, Uros</style></author><author><style face="normal" font="default" size="100%">Sergey, Gary</style></author><author><style face="normal" font="default" size="100%">Sesar, Branimir</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Siegmund, Walter A.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Szokoly, Gyula P.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Teodoro, Luis</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Walkowicz, Lucianne M.</style></author><author><style face="normal" font="default" size="100%">Wang, Shu-i.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilhite, Brian C.</style></author><author><style face="normal" font="default" size="100%">Xu, Yongzhong</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yasuda, Naoki</style></author><author><style face="normal" font="default" size="100%">Yip, Ching-Wa</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zibetti, Stefano</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Second Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AJ....128..502A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">128</style></volume><pages><style face="normal" font="default" size="100%">502-512</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Sloan Digital Sky Survey (SDSS) has validated and made publiclyavailable its Second Data Release. This data release consists of 3324deg&lt;sup&gt;2&lt;/sup&gt; of five-band (ugriz) imaging data with photometry forover 88 million unique objects, 367,360 spectra of galaxies, quasars,stars, and calibrating blank sky patches selected over 2627deg&lt;sup&gt;2&lt;/sup&gt; of this area, and tables of measured parameters from&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0403325</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Pavlovski, Krešimir</style></author><author><style face="normal" font="default" size="100%">Ilijić, Saša</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Second Stellar Color Locus: a Bridge from White Dwarfs to M stars</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...615L.141S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">615</style></volume><pages><style face="normal" font="default" size="100%">L141-L144</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of a locus of binary stars in the Sloan DigitalSky Survey (SDSS) g-r versus u-g color-color diagram that connects thecolors of white dwarfs and M dwarfs. While its contrast with respect tothe main stellar locus is only ~1:2300, this previously unrecognizedfeature includes 863 stars from the SDSS Data Release 1 (DR1). Theposition and shape of the feature are in good agreement with predictionsof a simple binary star model that consists of a white dwarf and an Mdwarf, with the components' luminosity ratio controlling the positionalong this binary system locus. SDSS DR1 spectra for 47 of these objectsstrongly support this model. The absolute magnitude-color distributioninferred for the white dwarf component is in good agreement with themodels of Bergeron et al.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0403218</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Quintero, Alejandro D.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Goto, Tomotsugu</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Selection and Photometric Properties of K+A Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...602..190Q</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">602</style></volume><pages><style face="normal" font="default" size="100%">190-199</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Two different simple measurements of galaxy star formation rate withdifferent timescales are compared empirically on 156,395 fiber spectraof galaxies with r&amp;lt;17.77 mag taken from the Sloan Digital Sky Surveyin the redshift range 0.05-4h&lt;sup&gt;3&lt;/sup&gt;Mpc&lt;sup&gt;-3&lt;/sup&gt;Gyr&lt;sup&gt;-1&lt;/sup&gt; atredshift z~0.1. These events are taking place in the field; the K+Agalaxies found in this study do not primarily lie in the high-densityenvironments or clusters typical of bulge-dominated populations.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0307074</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Sekiguchi, Maki</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Hayes, Jeffrey</style></author><author><style face="normal" font="default" size="100%">Kinney, Ellynne</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Briggs, John W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Covey, Kevin R.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Dong, Feng</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Gurbani, Vijay K.</style></author><author><style face="normal" font="default" size="100%">de Haas, Ernst</style></author><author><style face="normal" font="default" size="100%">Harris, Frederick H.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kniazev, Alexei Yu.</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Mannery, Ed</style></author><author><style face="normal" font="default" size="100%">Martínez-Delgado, David</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Pauls, George</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas R.</style></author><author><style face="normal" font="default" size="100%">Rafikov, R. R.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schroeder, Joshua</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Siegmund, Walter A.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szokoly, Gyula P.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">Yasuda, Naoki</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Sloan Digital Sky Survey Imaging of Low Galactic Latitude Fields: Technical Summary and Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AJ....128.2577F</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">128</style></volume><pages><style face="normal" font="default" size="100%">2577-2592</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Sloan Digital Sky Survey (SDSS) mosaic camera and telescope haveobtained five-band optical-wavelength imaging near the Galactic planeoutside of the nominal survey boundaries. These additional data wereobtained during commissioning and subsequent testing of the SDSSobserving system, and they provide unique wide-area imaging data inregions of high obscuration and star formation, including numerous youngstellar objects, Herbig-Haro objects, and young star clusters. Becausethese data are outside the survey regions in the Galactic caps, they arenot part of the standard SDSS data releases. This paper presents imagingdata for 832 square degrees of sky (including repeats), in thestar-forming regions of Orion, Taurus, and Cygnus. About 470deg&lt;sup&gt;2&lt;/sup&gt; are now released to the public, with the remainder tofollow at the time of SDSS Data Release 4. The public data in Orioninclude the star-forming region NGC 2068/NGC 2071/HH 24 and a large partof Barnard's loop.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0409700</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bolton, Adam S.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Sloan Digital Sky Survey Spectroscopic Lens Search. I. Discovery of Intermediate-Redshift Star-forming Galaxies behind Foreground Luminous Red Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AJ....127.1860B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">127</style></volume><pages><style face="normal" font="default" size="100%">1860-1882</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a catalog of 49 spectroscopic strong gravitational lenscandidates selected from a Sloan Digital Sky Survey sample of 50,996luminous red galaxies. Potentially lensed star-forming galaxies aredetected through the presence of background oxygen and hydrogen nebularemission lines in the spectra of these massive foreground galaxies. Thismultiline selection eliminates the ambiguity of single-lineidentification and provides a very promising sample of candidategalaxy-galaxy lens systems at low to intermediate redshift, withforeground redshifts ranging from 0.16 to 0.49 and background redshiftsfrom 0.25 to 0.81. Any lenses confirmed within our sample would beimportant new probes of early-type galaxy mass distributions, providingcomplementary constraints to those obtained from currently known lensedhigh-redshift quasars.Based in part on observations obtained with the 6.5 m Clay telescope ofthe Magellan Consortium.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0311055</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Haiman, Zoltán</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Snapshot Survey for Gravitational Lenses among z&gt;=4.0 Quasars. I. The z&gt;5.7 Sample</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004AJ....127.1305R</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">127</style></volume><pages><style face="normal" font="default" size="100%">1305-1312</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Over the last few years, the Sloan Digital Sky Survey (SDSS) hasdiscovered several hundred quasars with redshift between 4.0 and 6.4.Including the effects of magnification bias, one expects a priori thatan appreciable fraction of these objects are gravitationally lensed. Wehave used the Advanced Camera for Surveys on the Hubble Space Telescopeto carry out a snapshot imaging survey of high-redshift SDSS quasars tosearch for gravitationally split lenses. This paper, the first in aseries reporting the results of the survey, describes snapshotobservations of four quasars at z=5.74, 5.82, 5.99, and 6.30,respectively. We find that none of these objects has a lensed companionwithin 5 mag with a separation larger than 0.3&quot; within 2.5 mag we canrule out companions within 0.1&quot;. Based on the nondetection of stronglensing in these four systems, we constrain the z~6 luminosity functionto a slope of β&amp;gt;-4.63 (3 σ), assuming a break in thequasar luminosity function at M&lt;sup&gt;*&lt;/sup&gt;&lt;sub&gt;1450&lt;/sub&gt;=-24.1. Wediscuss the implications of this constraint on the ionizing backgrounddue to quasars in the early universe. Given that these quasars are nothighly magnified, estimates of the masses of their central engines bythe Eddington argument must be taken seriously, possibly challengingmodels of black hole formation.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0309274</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bouwens, R. J.</style></author><author><style face="normal" font="default" size="100%">Illingworth, G. D.</style></author><author><style face="normal" font="default" size="100%">Thompson, R. I.</style></author><author><style face="normal" font="default" size="100%">Blakeslee, J. P.</style></author><author><style face="normal" font="default" size="100%">Dickinson, M. E.</style></author><author><style face="normal" font="default" size="100%">Broadhurst, T. J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Fan, X.</style></author><author><style face="normal" font="default" size="100%">Franx, M.</style></author><author><style face="normal" font="default" size="100%">Meurer, G.</style></author><author><style face="normal" font="default" size="100%">van Dokkum, P.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Star Formation at z ~ 6: The Hubble Ultra Deep Parallel Fields</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...606L..25B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">606</style></volume><pages><style face="normal" font="default" size="100%">L25-L28</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report on the i-dropouts detected in two exceptionally deep AdvancedCamera for Surveys fields (B&lt;sub&gt;435&lt;/sub&gt;, V&lt;sub&gt;606&lt;/sub&gt;,i&lt;sub&gt;775&lt;/sub&gt;, and z&lt;sub&gt;850&lt;/sub&gt; with 10σ limits of 28.8,29.0, 28.5, and 27.8, respectively) taken in parallel with the UltraDeep Field Near-Infrared Camera and Multi-Object Spectrometerobservations. Using an i-z&amp;gt;1.4 cut, we find 30 i-dropouts over 21arcmin&lt;sup&gt;2&lt;/sup&gt; down to z&lt;sub&gt;850,AB&lt;/sub&gt;=28.1, or 1.4 i-dropoutsarcmin&lt;sup&gt;-2&lt;/sup&gt;, with significant field-to-field variation (asexpected from cosmic variance). This extends i-dropout searches some~0.9 mag further down the luminosity function than was possible in theGreat Observatories Origins Deep Survey (GOODS) fields, yielding a ~7times increase in surface density. An estimate of the size evolution forUV-bright objects is obtained by comparing the composite radial fluxprofile of the bright i-dropouts (z&lt;sub&gt;850,AB&lt;/sub&gt;&amp;lt;27.2) withscaled versions of the Hubble Deep Field-North and -South U-dropouts.The best fit is found with a(1+z)&lt;sup&gt;-1.57&lt;sup&gt;+0.50&lt;/sup&gt;&lt;sub&gt;-0.53&lt;/sub&gt;&lt;/sup&gt; scaling in size(for fixed luminosity), extending lower redshift (1-2.8 innumber and (1+z)&lt;sup&gt;0.1&lt;/sup&gt; in luminosity, suggesting a rest-framecontinuum UV luminosity density at z~6 that is just0.38&lt;sup&gt;+0.09&lt;/sup&gt;&lt;sub&gt;-0.07&lt;/sub&gt; times that at z~3.8. Our inclusionof the size evolution makes the present estimate lower than previous z~6estimates.Based on observations made with the NASA/ESA Hubble Space Telescope,which is operated by the Association of Universities for Research inAstronomy, Inc., under NASA contract NAS5-26555. These observations areassociated with program 9803.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1086/421016</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">White, Martin</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Theoretical uncertainty in baryon oscillations</style></title><secondary-title><style face="normal" font="default" size="100%">Physical Review D</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004PhRvD..70j3523E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">70</style></volume><pages><style face="normal" font="default" size="100%">103523</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We discuss the systematic uncertainties in the recovery of dark energyproperties from the use of baryon acoustic oscillations as a standardruler. We demonstrate that while unknown relativistic components in theuniverse prior to recombination would alter the sound speed, theinferences for dark energy from low-redshift surveys are unchanged solong as the microwave background anisotropies can measure the redshiftof matter-radiation equality, which they can do to sufficient accuracy.The mismeasurement of the radiation and matter densities themselves (asopposed to their ratio) would manifest as an incorrect prediction forthe Hubble constant at low-redshift. In addition, these anomalies doproduce subtle but detectable features in the microwave anisotropies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0407539</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Hoyle, Fiona</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Budavari, Tamás</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hamilton, Andrew J. S.</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Verde, Licia</style></author><author><style face="normal" font="default" size="100%">Xu, Yongzhong</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gott, J. Richard, III</style></author><author><style face="normal" font="default" size="100%">Hennessy, Greg</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Liam</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">{SDSS Collaboration}</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2004</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2004ApJ...606..702T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">606</style></volume><pages><style face="normal" font="default" size="100%">702-740</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We measure the large-scale real-space power spectrum P(k) by using asample of 205,443 galaxies from the Sloan Digital Sky Survey, covering2417 effective square degrees with mean redshift z~0.1. We employ amatrix-based method using pseudo-Karhunen-Loève eigenmodes,producing uncorrelated minimum-variance measurements in 22 k-bands ofboth the clustering power and its anisotropy due to redshift-spacedistortions, with narrow and well-behaved window functions in the range0.02hMpc&lt;sup&gt;-1&lt;/sup&gt;-1. We pay particularattention to modeling, quantifying, and correcting for potentialsystematic errors, nonlinear redshift distortions, and the artificialred-tilt caused by luminosity-dependent bias. Our results are robust toomitting angular and radial density fluctuations and are consistentbetween different parts of the sky. Our final result is a measurement ofthe real-space matter power spectrum P(k) up to an unknown overallmultiplicative bias factor. Our calculations suggest that this biasfactor is independent of scale to better than a few percent fork&amp;lt;0.1hMpc&lt;sup&gt;-1&lt;/sup&gt;, thereby making our results useful forprecision measurements of cosmological parameters in conjunction withdata from other experiments such as the Wilkinson Microwave AnisotropyProbe satellite. The power spectrum is not well-characterized by asingle power law but unambiguously shows curvature. As a simplecharacterization of the data, our measurements are well fitted by a flatscale-invariant adiabatic cosmological model withhΩ&lt;sub&gt;m&lt;/sub&gt;=0.213+/-0.023 and σ&lt;sub&gt;8&lt;/sub&gt;=0.89+/-0.02for L&lt;sub&gt;*&lt;/sub&gt; galaxies, when fixing the baryon fractionΩ&lt;sub&gt;b&lt;/sub&gt;/Ω&lt;sub&gt;m&lt;/sub&gt;=0.17 and the Hubble parameterh=0.72; cosmological interpretation is given in a companion paper.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0310725</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon N.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Angular Clustering with Photometric Redshifts in the Sloan Digital Sky Survey: Bimodality in the Clustering Properties of Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...595...59B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">595</style></volume><pages><style face="normal" font="default" size="100%">59-70</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Understanding the clustering of galaxies has long been a goal of modernobservational cosmology. Redshift surveys have been used to measure thecorrelation length as a function of luminosity and color. However, whensubdividing the catalogs into multiple subsets, the errors increaserapidly. Angular clustering in magnitude-limited photometric surveys hasthe advantage of much larger catalogs but suffers from a dilution of theclustering signal because of the broad radial distribution of thesample. Also, up to now it has not been possible to select uniformsubsamples based on physical parameters, such as luminosity andrest-frame color. Utilizing our photometric redshift technique, avolume-limited sample (0.10=5.77+/-0.10h&lt;sup&gt;-1&lt;/sup&gt;Mpc. We find that r&lt;sub&gt;0&lt;/sub&gt;increases with luminosity by a factor of 1.6 over the sampled luminosityrange, in agreement with previous redshift surveys. We also find thatboth the clustering length and the slope of the correlation functiondepend on the galaxy type. In particular, by splitting the galaxies infour groups by their rest-frame type, we find a bimodal behavior intheir clustering properties. Galaxies with spectral types similar toelliptical galaxies have a correlation length of6.59+/-0.17h&lt;sup&gt;-1&lt;/sup&gt;Mpc and a slope of the angular correlationfunction of 0.96+/-0.05, while blue galaxies have a clustering length of4.51+/-0.19h&lt;sup&gt;-1&lt;/sup&gt;Mpc and a slope of 0.68+/-0.09. The twointermediate color groups behave like their more extreme ``siblings''rather than showing a gradual transition in slope. We discuss thesecorrelations in the context of current cosmological models for structureformation.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0305603</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Győry, Zsuzsanna</style></author><author><style face="normal" font="default" size="100%">Benítez, Narciso</style></author><author><style face="normal" font="default" size="100%">Annis, Jim</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, Jim</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Application of Photometric Redshifts to the SDSS Early Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">February 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....125..580C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">125</style></volume><pages><style face="normal" font="default" size="100%">580-592</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Early Data Release (EDR) from the Sloan Digital Sky Survey providesone of the largest multicolor photometric catalogs currently availableto the astronomical community. In this paper we present the firstapplication of photometric redshifts to the ~6 million extended sourcesin these data (with 1.8 million sources having r'&amp;lt;21). Utilizing arange of photometric redshift techniques, from empirical to template andhybrid techniques, we investigate the statistical and systematicuncertainties present in the redshift estimates for the EDR data. Forr'&amp;lt;21, we find that the redshift estimates provide realistic redshifthistograms with an rms uncertainty in the photometric redshift relationof 0.035 at r'&amp;lt;18 and rising to 0.1 at r'&amp;lt;21. We conclude bydescribing how these photometric redshifts and derived quantities, suchas spectral type, rest-frame colors, and absolute magnitudes, are storedin the SDSS database. We provide sample queries for searching onphotometric redshifts and list the current caveats and issues thatshould be understood before using these photometric redshifts instatistical analyses of the SDSS galaxies.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0211080</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Nakamura, Osamu</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alex</style></author><author><style face="normal" font="default" size="100%">York, Don G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Average Spectra of Massive Galaxies in the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...585..694E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">585</style></volume><pages><style face="normal" font="default" size="100%">694-713</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We combine Sloan Digital Sky Survey spectra of 22,000 luminous, red,bulge-dominated galaxies to get high signal-to-noise ratio averagespectra in the rest-frame optical and ultraviolet (2600-7000 Å).The average spectra of these massive, quiescent galaxies are early typewith weak emission lines and with absorption lines indicating anapparent excess of α-elements over solar abundance ratios. We makeaverage spectra of subsamples selected by luminosity, environment, andredshift. The average spectra are remarkable in their similarity. Whatvariations do exist in the average spectra as a function of luminosityand environment are found to form a nearly one-parameter family inspectrum space. We present a high signal-to-noise ratio spectrum of thevariation. We measure the properties of the variation with a modifiedversion of the Lick index system and compare to model spectra fromstellar population syntheses. The variation may be a combination of ageand chemical abundance differences, but the conservative conclusion isthat the quality of the data considerably exceeds the current state ofthe models.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0212087</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Lamb, D. Q.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazuhiro</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Broadband Optical Properties of Galaxies with Redshifts 0.02&lt;z&lt;0.22</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...594..186B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">594</style></volume><pages><style face="normal" font="default" size="100%">186-207</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Using photometry and spectroscopy of 183,487 galaxies from the SloanDigital Sky Survey, we present bivariate distributions of pairs of sevengalaxy properties: four optical colors, surface brightness, radialprofile shape as measured by the Sérsic index, and absolutemagnitude. In addition, we present the dependence of local galaxydensity (smoothed on 8 h&lt;sup&gt;-1&lt;/sup&gt; Mpc scales) on all of theseproperties. Several classic, well-known relations among galaxyproperties are evident at extremely high signal-to-noise ratio: thecolor-color relations of galaxies, the color-magnitude relations, themagnitude-surface brightness relation, and the dependence of density oncolor and absolute magnitude. We show that most of the i-band luminositydensity in the universe is in the absolute magnitude and surfacebrightness ranges used: -23.50.1&lt;sub&gt;i&lt;/sub&gt;&amp;lt;-17.0mag and 17&amp;lt;μ&lt;sub&gt;0.1&lt;sub&gt;i&lt;/sub&gt;&lt;/sub&gt;&amp;lt;24 mag in 1arcsec&lt;sup&gt;2&lt;/sup&gt; [the notation &lt;sup&gt;z&lt;/sup&gt;b represents the b bandshifted blueward by a factor (1+z)]. Some of the relationships betweenparameters, in particular the color-magnitude relations, show strongercorrelations for exponential galaxies and concentrated galaxies takenseparately than for all galaxies taken together. We provide a simple setof fits of the dependence of galaxy properties on luminosity for thesetwo sets of galaxies and other quantitative details of our results.Based on observations obtained with the Sloan Digital Sky Survey.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0209479</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Deprojecting Densities from Angular Cross-Correlations</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...586..718E</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">586</style></volume><pages><style face="normal" font="default" size="100%">718-722</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present a model-independent, spherically symmetric density estimatorto be used in the cross-correlation of imaging catalogs with objects ofknown redshift. The estimator is a simple modification of the usualprojected density estimator, with weightings that produce a sphericalaperture rather than a cylindrical one.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0212084</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Blakeslee, John P.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Early-Type Galaxies in the Sloan Digital Sky Survey. I. The Sample</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....125.1817B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">125</style></volume><pages><style face="normal" font="default" size="100%">1817-1848</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;A sample of nearly 9000 early-type galaxies, in the redshift range0.01&amp;lt;=z&amp;lt;=0.3, was selected from the Sloan Digital Sky Survey(SDSS) using morphological and spectral criteria. This paper describeshow the sample was selected, presents examples of images andseeing-corrected fits to the observed surface brightness profiles,describes our method for estimating K-corrections, and shows that theSDSS spectra are of sufficiently high quality to measure velocitydispersions accurately. It also provides catalogs of the measuredphotometric and spectroscopic parameters. In related papers, these dataare used to study how early-type galaxy observables, includingluminosity, effective radius, surface brightness, color, and velocitydispersion, are correlated with one another.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0301631</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Blakeslee, John P.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Early-type Galaxies in the Sloan Digital Sky Survey. II. Correlations between Observables</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....125.1849B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">125</style></volume><pages><style face="normal" font="default" size="100%">1849-1865</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;A magnitude-limited sample of nearly 9000 early-type galaxies, in theredshift range 0.01&amp;lt;=z&amp;lt;=0.3, was selected from the Sloan DigitalSky Survey using morphological and spectral criteria. The sample wasused to study how early-type galaxy observables, including luminosity L,effective radius R&lt;sub&gt;o&lt;/sub&gt;, surface brightness I&lt;sub&gt;o&lt;/sub&gt;, color,and velocity dispersion σ, are correlated with one another.Measurement biases are understood with mock catalogs that reproduce allof the observed scaling relations and their dependences on fittingtechnique. At any given redshift, the intrinsic distribution ofluminosities, sizes, and velocity dispersions in our sample are allapproximately Gaussian. A maximum likelihood analysis shows thatσ~L&lt;sup&gt;0.25+/-0.012&lt;/sup&gt;,R&lt;sub&gt;o&lt;/sub&gt;~L&lt;sup&gt;0.63+/-0.025&lt;/sup&gt;, andR&lt;sub&gt;o&lt;/sub&gt;~I&lt;sup&gt;-0.75+/-0.02&lt;/sup&gt; in the r* band. In addition, themass-to-light ratio within the effective radius scales asM&lt;sub&gt;o&lt;/sub&gt;/L~L&lt;sup&gt;0.14+/-0.02&lt;/sup&gt; orM&lt;sub&gt;o&lt;/sub&gt;/L~M&lt;sup&gt;0.22+/-0.05&lt;/sup&gt;&lt;sub&gt;o&lt;/sub&gt;, and galaxies withlarger effective masses have smaller effective densities:Δ&lt;sub&gt;o&lt;/sub&gt;~M&lt;sup&gt;-0.52+/-0.03&lt;/sup&gt;&lt;sub&gt;o&lt;/sub&gt;. Theserelations are approximately the same in the g*, i*, and z* bands.Relative to the population at the median redshift in the sample,galaxies at lower and higher redshifts have evolved only little, withmore evolution in the bluer bands. The luminosity function is consistentwith weak passive luminosity evolution and a formation time of about 9Gyr ago.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0301624</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Blakeslee, John P.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Early-Type Galaxies in the Sloan Digital Sky Survey. III. The Fundamental Plane</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">April 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....125.1866B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">125</style></volume><pages><style face="normal" font="default" size="100%">1866-1881</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;A magnitude-limited sample of nearly 9000 early-type galaxies in theredshift range 0.01&amp;lt;=z&amp;lt;=0.3 was selected from the Sloan DigitalSky Survey (SDSS) using morphological and spectral criteria. Thefundamental plane relation in this sample isR&lt;sub&gt;o&lt;/sub&gt;~σ&lt;sup&gt;1.49+/-0.05&lt;/sup&gt;I&lt;sup&gt;-0.75+/-0.01&lt;/sup&gt;&lt;sub&gt;o&lt;/sub&gt;in the r* band. It is approximately the same in the g*, i*, and z*bands. Relative to the population at the median redshift in the sample,galaxies at lower and higher redshifts have evolved only a little. Ifthe fundamental plane is used to quantify this evolution, then theapparent magnitude limit can masquerade as evolution; once thisselection effect has been accounted for, the evolution is consistentwith that of a passively evolving population that formed the bulk of itsstars about 9 Gyr ago. One of the principal advantages of the SDSSsample over previous samples is that the galaxies in it lie inenvironments ranging from isolation in the field to the dense cores ofclusters. The fundamental plane shows that galaxies in dense regions areslightly different from galaxies in less dense regions.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0301626</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Estimating Fixed-Frame Galaxy Magnitudes in the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....125.2348B</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">125</style></volume><pages><style face="normal" font="default" size="100%">2348-2360</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Broadband measurements of flux for galaxies at different redshiftsmeasure different regions of the rest-frame galaxy spectrum. Certainastronomical questions, such as the evolution of the luminosity functionof galaxies, require transforming these inherently redshift-dependentmagnitudes into redshift-independent quantities. To prepare to addressthese astronomical questions, investigated in detail in subsequentpapers, we fit spectral energy distributions (SEDs) to broadbandphotometric observations in the context of the optical observations ofthe Sloan Digital Sky Survey (SDSS). Linear combinations of fourspectral templates can reproduce the five SDSS magnitudes of allgalaxies to the precision of the photometry. Expressed in theappropriate coordinate system, the locus of the coefficients multiplyingthe templates is planar and, in fact, nearly linear. The resultingreconstructed SEDs can be used to recover fixed-frame magnitudes over arange of redshifts. This process yields consistent results in the sensethat, within each sample, the intrinsic colors of similar type galaxiesare nearly constant with redshift. We compare our results with simplerinterpolation methods and galaxy spectrophotometry from the SDSS. Thesoftware that generates these results is publicly available and easilyadapted to handle a wide range of galaxy observations.Based on observations obtained with the Sloan Digital Sky Survey.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0205243</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Abazajian, Kevork</style></author><author><style face="normal" font="default" size="100%">Adelman-McCarthy, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Agüeros, Marcel A.</style></author><author><style face="normal" font="default" size="100%">Allam, Sahar S.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Baldry, Ivan K.</style></author><author><style face="normal" font="default" size="100%">Bastian, Steven</style></author><author><style face="normal" font="default" size="100%">Berlind, Andreas</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Blythe, Norman</style></author><author><style face="normal" font="default" size="100%">Bochanski, John J., Jr.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brewington, Howard</style></author><author><style face="normal" font="default" size="100%">Briggs, John W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert J.</style></author><author><style face="normal" font="default" size="100%">Budavári, Tamás</style></author><author><style face="normal" font="default" size="100%">Carey, Larry N.</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Collinge, Matthew J.</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Covey, Kevin R.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Dalcanton, Julianne J.</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Dong, Feng</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Feldman, Paul D.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott D.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gal, Roy R.</style></author><author><style face="normal" font="default" size="100%">Gillespie, Bruce</style></author><author><style face="normal" font="default" size="100%">Glazebrook, Karl</style></author><author><style face="normal" font="default" size="100%">Gonzalez, Carlos F.</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Grebel, Eva K.</style></author><author><style face="normal" font="default" size="100%">Grodnicki, Lauren</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Gurbani, Vijay K.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Hao, Lei</style></author><author><style face="normal" font="default" size="100%">Harbeck, Daniel</style></author><author><style face="normal" font="default" size="100%">Harris, Frederick H.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne L.</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Helmboldt, J. F.</style></author><author><style face="normal" font="default" size="100%">Hendry, John S.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Holmgren, Donald J.</style></author><author><style face="normal" font="default" size="100%">Holtzman, Jon A.</style></author><author><style face="normal" font="default" size="100%">Homer, Lee</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Takashi</style></author><author><style face="normal" font="default" size="100%">Inkmann, John P.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Jordan, Beatrice</style></author><author><style face="normal" font="default" size="100%">Jordan, Wendell P.</style></author><author><style face="normal" font="default" size="100%">Jorgensen, Anders M.</style></author><author><style face="normal" font="default" size="100%">Jurić, Mario</style></author><author><style face="normal" font="default" size="100%">Kauffmann, Guinevere</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, G. R.</style></author><author><style face="normal" font="default" size="100%">Kniazev, Alexei Y.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard G.</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter Z.</style></author><author><style face="normal" font="default" size="100%">Kuropatkin, Nickolai</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lampeitl, Hubert</style></author><author><style face="normal" font="default" size="100%">Laubscher, Bryan E.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Li, Nolan</style></author><author><style face="normal" font="default" size="100%">Lidz, Adam</style></author><author><style face="normal" font="default" size="100%">Lin, Huan</style></author><author><style face="normal" font="default" size="100%">Loh, Yeong-Shang</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Malik, Tanu</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">McGehee, Peregrine M.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Miknaitis, Gajus A.</style></author><author><style face="normal" font="default" size="100%">Moorthy, Bhasker K.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Murphy, Tara</style></author><author><style face="normal" font="default" size="100%">Nakajima, Reiko</style></author><author><style face="normal" font="default" size="100%">Narayanan, Vijay K.</style></author><author><style face="normal" font="default" size="100%">Nash, Thomas</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Nieto-Santisteban, Maria</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Odenkirchen, Michael</style></author><author><style face="normal" font="default" size="100%">Okamura, Sadanori</style></author><author><style face="normal" font="default" size="100%">Ostriker, Jeremiah P.</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Padmanabhan, Nikhil</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian C.</style></author><author><style face="normal" font="default" size="100%">Quinn, Thomas R.</style></author><author><style face="normal" font="default" size="100%">Rafikov, R. R.</style></author><author><style face="normal" font="default" size="100%">Raymond, Sean N.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schaye, Joop</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Schroeder, Joshua</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sekiguchi, Maki</style></author><author><style face="normal" font="default" size="100%">Seljak, Uroš</style></author><author><style face="normal" font="default" size="100%">Sergey, Gary</style></author><author><style face="normal" font="default" size="100%">Sesar, Branimir</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin</style></author><author><style face="normal" font="default" size="100%">Shimasaku, Kazu</style></author><author><style face="normal" font="default" size="100%">Siegmund, Walter A.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Sinisgalli, Allan J.</style></author><author><style face="normal" font="default" size="100%">Sirko, Edwin</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Smolčić, Vernesa</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Steinhardt, Charles</style></author><author><style face="normal" font="default" size="100%">Stinson, Gregory</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strateva, Iskra V.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Tasca, Lidia</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Vandenberg, Jan</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Vogt, Nicole P.</style></author><author><style face="normal" font="default" size="100%">Walkowicz, Lucianne M.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">West, Andrew A.</style></author><author><style face="normal" font="default" size="100%">White, Simon D. M.</style></author><author><style face="normal" font="default" size="100%">Wilhite, Brian C.</style></author><author><style face="normal" font="default" size="100%">Willman, Beth</style></author><author><style face="normal" font="default" size="100%">Xu, Yongzhong</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Yarger, Jean</style></author><author><style face="normal" font="default" size="100%">Yasuda, Naoki</style></author><author><style face="normal" font="default" size="100%">Yip, Ching-Wa</style></author><author><style face="normal" font="default" size="100%">Yocum, D. R.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">Zakamska, Nadia L.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Zheng, Wei</style></author><author><style face="normal" font="default" size="100%">Zibetti, Stefano</style></author><author><style face="normal" font="default" size="100%">Zucker, Daniel B.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The First Data Release of the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....126.2081A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">126</style></volume><pages><style face="normal" font="default" size="100%">2081-2086</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Sloan Digital Sky Survey (SDSS) has validated and made publiclyavailable its First Data Release. This consists of 2099 deg&lt;sup&gt;2&lt;/sup&gt;of five-band (u,g,r,i,z) imaging data, 186,240 spectra of galaxies,quasars, stars and calibrating blank sky patches selected over 1360deg&lt;sup&gt;2&lt;/sup&gt; of this area, and tables of measured parameters fromthese data. The imaging data go to a depth of r~22.6 and are&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0305492</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Oguri, Masamune</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Hennawi, Joseph F.</style></author><author><style face="normal" font="default" size="100%">Chiu, Kuenley</style></author><author><style face="normal" font="default" size="100%">Zheng, Wei</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Shin-ichi</style></author><author><style face="normal" font="default" size="100%">Gregg, Michael D.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Suto, Yasushi</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Turner, Edwin L.</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen M.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rix, Hans-Walter</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin Scott</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A gravitationally lensed quasar with quadruple images separated by 14.62arcseconds</style></title><secondary-title><style face="normal" font="default" size="100%">Nature</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003Natur.426..810I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">426</style></volume><pages><style face="normal" font="default" size="100%">810-812</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Gravitational lensing is a powerful tool for the study of thedistribution of dark matter in the Universe. The cold-dark-matter modelof the formation of large-scale structures (that is, clusters ofgalaxies and even larger assemblies) predicts the existence of quasarsgravitationally lensed by concentrations of dark matter so massive thatthe quasar images would be split by over 7arcsec. Numerous searches forlarge-separation lensed quasars have, however, been unsuccessful. All ofthe roughly 70 lensed quasars known, including the first lensed quasardiscovered, have smaller separations that can be explained in terms ofgalaxy-scale concentrations of baryonic matter. Although gravitationallylensed galaxies with large separations are known, quasars are moreuseful cosmological probes because of the simplicity of the resultinglens systems. Here we report the discovery of a lensed quasar, SDSSJ1004 + 4112, which has a maximum separation between the components of14.62arcsec. Such a large separation means that the lensing object mustbe dominated by dark matter. Our results are fully consistent withtheoretical expectations based on the cold-dark-matter model.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0312427</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Schmidt, Gary</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Dan</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Collinge, Matthew J.</style></author><author><style face="normal" font="default" size="100%">Dahn, Conard C.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert</style></author><author><style face="normal" font="default" size="100%">Ivezić, Zeljko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">An Initial Survey of White Dwarfs in the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....126.1023H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">126</style></volume><pages><style face="normal" font="default" size="100%">1023-1040</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;An initial assessment is made of white dwarf and hot subdwarf starsobserved in the Sloan Digital Sky Survey. In a small area of sky (190square degrees), observed much like the full survey will be, 269 whitedwarfs (WDs) and 56 hot subdwarfs are identified spectroscopically whereonly 44 white dwarfs and five hot subdwarfs were known previously. Mostare ordinary DA (hydrogen atmosphere) and DB (helium) types. Inaddition, in the full survey to date, a number of WDs have been foundwith uncommon spectral types. Among these are blue DQ stars displayinglines of atomic carbon; red DQ stars showing molecular bands ofC&lt;sub&gt;2&lt;/sub&gt; with a wide variety of strengths; DZ stars where Ca andoccasionally Mg, Na, and/or Fe lines are detected; and magnetic WDs witha wide range of magnetic field strengths in DA, DB, DQ, and (probably)DZ spectral types. Photometry alone allows identification of starshotter than 12,000 K, and the density of these stars for 15-2 at Galactic latitudes of29°-62°. Spectra are obtained for roughly half of these hot&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0305347</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Matsubara, Takahiko</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Kerscher, Martin</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Narayanan, Vijay</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Liam</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Hennessy, Greg</style></author><author><style face="normal" font="default" size="100%">Ivezic, Zeljko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter Z.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author><author><style face="normal" font="default" size="100%">{SDSS Collaboration}</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Karhunen-Loève Estimation of the Power Spectrum Parameters from the Angular Distribution of Galaxies in Early Sloan Digital Sky Survey Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...591....1S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">591</style></volume><pages><style face="normal" font="default" size="100%">1-11</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present measurements of parameters of the three-dimensional powerspectrum of galaxy clustering from 222 square degrees of early imagingdata in the Sloan Digital Sky Survey (SDSS). The projected galaxydistribution on the sky is expanded over a set of Karhunen-Loève(KL) eigenfunctions, which optimize the signal-to-noise ratio in ouranalysis. A maximum likelihood analysis is used to estimate parametersthat set the shape and amplitude of the three-dimensional power spectrumof galaxies in the SDSS magnitude-limited sample withr&lt;sup&gt;*&lt;/sup&gt;&amp;lt;21. Our best estimates are Γ=0.188+/-0.04 andσ&lt;sub&gt;8L&lt;/sub&gt;=0.915+/-0.06 (statistical errors only), for a flatuniverse with a cosmological constant. We demonstrate that ourmeasurements contain signal from scales at or beyond the peak of thethree-dimensional power spectrum. We discuss how the results scale withsystematic uncertainties, like the radial selection function. We findthat the central values satisfy the analytically estimated scalingrelation. We have also explored the effects of evolutionary corrections,various truncations of the KL basis, seeing, sample size, and limitingmagnitude. We find that the impact of most of these uncertainties staywithin the 2 σ uncertainties of our fiducial result.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0107419</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Schmidt, Gary D.</style></author><author><style face="normal" font="default" size="100%">Harris, Hugh C.</style></author><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Harvanek, Michael</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Krzesinski, Jurek</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Long, Dan</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H.</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole M.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Snedden, Stephanie A.</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Dan</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Magnetic White Dwarfs from the Sloan Digital Sky Survey: The First Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">October 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...595.1101S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">595</style></volume><pages><style face="normal" font="default" size="100%">1101-1113</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;Beyond its goals related to the extragalactic universe, the SloanDigital Sky Survey (SDSS) is an effective tool for identifying stellarobjects with unusual spectral energy distributions. Here we report onthe 53 new magnetic white dwarfs discovered during the first two yearsof the survey, including 38 whose data are made public in the 1500deg&lt;sup&gt;2&lt;/sup&gt; First Data Release. Discoveries span the magnitude range16.3&amp;lt;=g&amp;lt;=20.5, and based on the recovery rate for previously knownmagnetic white dwarfs, the completeness of the SDSS appears to be highfor reasonably hot stars with B&amp;gt;~3 MG and g&amp;gt;~15. The new objectsnearly double the total number of known magnetic white dwarfs andinclude examples with polar field strengths B&lt;sub&gt;p&lt;/sub&gt;&amp;gt;500 MG, aswell as several with exotic atmospheric compositions. The improvedsample statistics and uniformity indicate that the distribution ofmagnetic white dwarfs has a broad peak in the range ~5-30 MG and a tailextending to nearly 10&lt;sup&gt;9&lt;/sup&gt; G. Degenerates with polar fieldsB&lt;sub&gt;p&lt;/sub&gt;&amp;gt;~50 MG are consistent with being descendents ofmagnetic Ap/Bp main-sequence stars, but low- and moderate-field magneticwhite dwarfs appear to imply another origin. Yet-undetected magneticF-type stars with convective envelopes that destroy the orderedunderlying field are attractive candidates.A portion of the results presented here were obtained with the MMTObservatory, a facility operated jointly by the University of Arizonaand the Smithsonian Institution.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0307121</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Hogg, David W.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Overdensities of Galaxy Environments as a Function of Luminosity and Color</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">March 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...585L...5H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">585</style></volume><pages><style face="normal" font="default" size="100%">L5-L9</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We study the mean environments of galaxies in the Sloan Digital SkySurvey (SDSS) as a function of rest-frame luminosity and color.Overdensities in galaxy number are estimated in 8 and 1 h&lt;sup&gt;-1&lt;/sup&gt;Mpc spheres centered on 115,000 galaxies taken from the SDSSspectroscopic sample. We find that, at constant color, overdensity isindependent of luminosity for galaxies with the blue colors of spirals.This suggests that at fixed star formation history, spiral-galaxy massis a very weak function of environment. Overdensity does depend onluminosity for galaxies with the red colors of early types; bothlow-luminosity and high-luminosity red galaxies are found to be inhighly overdense regions.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0212085</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Matheson, T.</style></author><author><style face="normal" font="default" size="100%">Garnavich, P. M.</style></author><author><style face="normal" font="default" size="100%">Stanek, K. Z.</style></author><author><style face="normal" font="default" size="100%">Bersier, D.</style></author><author><style face="normal" font="default" size="100%">Holland, S. T.</style></author><author><style face="normal" font="default" size="100%">Krisciunas, K.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Berlind, P.</style></author><author><style face="normal" font="default" size="100%">Bloom, J. S.</style></author><author><style face="normal" font="default" size="100%">Bolte, M.</style></author><author><style face="normal" font="default" size="100%">Bonanos, A. Z.</style></author><author><style face="normal" font="default" size="100%">Brown, M. J. I.</style></author><author><style face="normal" font="default" size="100%">Brown, W. R.</style></author><author><style face="normal" font="default" size="100%">Calkins, M. L.</style></author><author><style face="normal" font="default" size="100%">Challis, P.</style></author><author><style face="normal" font="default" size="100%">Chornock, R.</style></author><author><style face="normal" font="default" size="100%">Echevarria, L.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Everett, M. E.</style></author><author><style face="normal" font="default" size="100%">Filippenko, A. V.</style></author><author><style face="normal" font="default" size="100%">Flint, K.</style></author><author><style face="normal" font="default" size="100%">Foley, R. J.</style></author><author><style face="normal" font="default" size="100%">Freedman, D. L.</style></author><author><style face="normal" font="default" size="100%">Hamuy, Mario</style></author><author><style face="normal" font="default" size="100%">Harding, P.</style></author><author><style face="normal" font="default" size="100%">Hathi, N. P.</style></author><author><style face="normal" font="default" size="100%">Hicken, M.</style></author><author><style face="normal" font="default" size="100%">Hoopes, C.</style></author><author><style face="normal" font="default" size="100%">Impey, C.</style></author><author><style face="normal" font="default" size="100%">Jannuzi, B. T.</style></author><author><style face="normal" font="default" size="100%">Jansen, R. A.</style></author><author><style face="normal" font="default" size="100%">Jha, S.</style></author><author><style face="normal" font="default" size="100%">Kaluzny, J.</style></author><author><style face="normal" font="default" size="100%">Kannappan, S.</style></author><author><style face="normal" font="default" size="100%">Kirshner, R. P.</style></author><author><style face="normal" font="default" size="100%">Latham, D. W.</style></author><author><style face="normal" font="default" size="100%">Lee, J. C.</style></author><author><style face="normal" font="default" size="100%">Leonard, D. C.</style></author><author><style face="normal" font="default" size="100%">Li, W.</style></author><author><style face="normal" font="default" size="100%">Luhman, K. L.</style></author><author><style face="normal" font="default" size="100%">Martini, P.</style></author><author><style face="normal" font="default" size="100%">Mathis, H.</style></author><author><style face="normal" font="default" size="100%">Maza, J.</style></author><author><style face="normal" font="default" size="100%">Megeath, S. T.</style></author><author><style face="normal" font="default" size="100%">Miller, L. R.</style></author><author><style face="normal" font="default" size="100%">Minniti, D.</style></author><author><style face="normal" font="default" size="100%">Olszewski, E. W.</style></author><author><style face="normal" font="default" size="100%">Papenkova, M.</style></author><author><style face="normal" font="default" size="100%">Phillips, M. M.</style></author><author><style face="normal" font="default" size="100%">Pindor, B.</style></author><author><style face="normal" font="default" size="100%">Sasselov, D. D.</style></author><author><style face="normal" font="default" size="100%">Schild, R.</style></author><author><style face="normal" font="default" size="100%">Schweiker, H.</style></author><author><style face="normal" font="default" size="100%">Spahr, T.</style></author><author><style face="normal" font="default" size="100%">Thomas-Osip, J.</style></author><author><style face="normal" font="default" size="100%">Thompson, I.</style></author><author><style face="normal" font="default" size="100%">Weisz, D.</style></author><author><style face="normal" font="default" size="100%">Windhorst, R.</style></author><author><style face="normal" font="default" size="100%">Zaritsky, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Photometry and Spectroscopy of GRB 030329 and Its Associated Supernova 2003dh: The First Two Months</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...599..394M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">599</style></volume><pages><style face="normal" font="default" size="100%">394-407</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present extensive optical and infrared photometry of the afterglow ofgamma-ray burst (GRB) 030329 and its associated supernova (SN) 2003dhover the first two months after detection (2003 March 30-May 29 UT).Optical spectroscopy from a variety of telescopes is shown and, whencombined with the photometry, allows an unambiguous separation betweenthe afterglow and SN contributions. The optical afterglow of the GRB isinitially a power-law continuum but shows significant color variationsduring the first week that are unrelated to the presence of an SN. Theearly afterglow light curve also shows deviations from the typicalpower-law decay. An SN spectrum is first detectable ~7 days after theburst and dominates the light after ~11 days. The spectral evolution andthe light curve are shown to closely resemble those of SN 1998bw, apeculiar Type Ic SN associated with GRB 980425, and the time of the SNexplosion is close to the observed time of the GRB. It is now clear thatat least some GRBs arise from core-collapse SNe.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0307435</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Seo, Hee-Jong</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...598..720S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">598</style></volume><pages><style face="normal" font="default" size="100%">720-740</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We show that the measurement of the baryonic acoustic oscillations inlarge high-redshift galaxy surveys offers a precision route to themeasurement of dark energy. The cosmic microwave background provides thescale of the oscillations as a standard ruler that can be measured inthe clustering of galaxies, thereby yielding the Hubble parameter andangular diameter distance as a function of redshift. This, in turn,enables one to probe dark energy. We use a Fisher matrix formalism tostudy the statistical errors for redshift surveys up to z=3 and reporterrors on cosmography while marginalizing over a large number ofcosmological parameters, including a time-dependent equation of state.With redshift surveys combined with cosmic microwave backgroundsatellite data, we achieve errors of 0.037 on Ω&lt;sub&gt;X&lt;/sub&gt;, 0.10on w(z=0.8), and 0.28 on dw(z)/dz for the cosmological constant model.Models with less negative w(z) permit tighter constraints. We test anddiscuss the dependence of performance on redshift, survey conditions,and the fiducial model. We find results that are competitive with theperformance of future Type Ia supernova surveys. We conclude thatredshift surveys offer a promising independent route to the measurementof dark energy.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0307460</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Keeton, Charles R.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">White, Richard L.</style></author><author><style face="normal" font="default" size="100%">Johnson, Eric T.</style></author><author><style face="normal" font="default" size="100%">Ma, Zhaoming</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Sheldon, Erin S.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J090334.92+502819.2: A New Gravitational Lens</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....126.2281J</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">126</style></volume><pages><style face="normal" font="default" size="100%">2281-2290</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of a new gravitationally lensed quasar from theSloan Digital Sky Survey, SDSS J090334.92+502819.2. This object wastargeted for SDSS spectroscopy as a luminous red galaxy, but manualexamination of the spectrum showed the presence of a quasar at z~=3.6 inaddition to a red galaxy at z=0.388, and the SDSS image showed a secondpossible quasar image nearby. Follow-up imaging and spectroscopyconfirmed the lensing hypothesis. In images taken at the AstrophysicalResearch Consortium 3.5 m telescope, two quasars are separated by 2.8&quot;the lensing galaxy is clearly seen and is blended with one of the quasarimages. Spectroscopy taken at the Keck II telescope shows that thequasars have identical redshifts of z~=3.6, and both show the presenceof the same broad absorption line-like troughs. We present simple lensmodels that account for the geometry and magnifications. The lens galaxylies near two groups of galaxies and may be a part of them. The modelssuggest that the groups may contribute considerable shear that has astrong effect on the lens configuration.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0307371</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Inada, Naohisa</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Johnston, David E.</style></author><author><style face="normal" font="default" size="100%">Pindor, Bartosz</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Schechter, Paul L.</style></author><author><style face="normal" font="default" size="100%">Sekiguchi, Maki</style></author><author><style face="normal" font="default" size="100%">White, Richard L.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Neilsen, Eric H., Jr.</style></author><author><style face="normal" font="default" size="100%">Newman, Peter R.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Snedden, S.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS J092455.87+021924.9: An Interesting Gravitationally Lensed Quasar from the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">August 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....126..666I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">126</style></volume><pages><style face="normal" font="default" size="100%">666-674</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We report the discovery of a new gravitationally lensed quasar from theSloan Digital Sky Survey, SDSS J092455.87+021924.9 (SDSS J0924+0219).This object was selected from among known SDSS quasars by an algorithmthat was designed to select another known SDSS lensed quasar (SDSSJ1226-0006A,B). Five separate components, three of which are unresolved,are identified in photometric follow-up observations obtained with theMagellan Consortium's 6.5 m Walter Baade Telescope at Las CampanasObservatory. Two of the unresolved components (designated A and B) areconfirmed to be quasars with z=1.524; the velocity difference is lessthan 100 km s&lt;sup&gt;-1&lt;/sup&gt; according to spectra taken with the W. M.Keck Observatory's Keck II Telescope at Mauna Kea, Hawaii. A thirdstellar component, designated C, has the colors of a quasar withredshift similar to components A and B. The maximum separation of thepoint sources is 1.78&quot;. The other two sources, designated G and D, areresolved. Component G appears to be the best candidate for the lensinggalaxy. Although component D is near the expected position of the fourthlensed component in a four-image lens system, its properties are notconsistent with being the image of a quasar at z~1.5. Nevertheless, theidentical redshifts of components A and B and the presence of componentC strongly suggest that this object is a gravitational lens. Ourobservations support the idea that a foreground object reddens thefourth lensed component and that another unmodeled effect (such asmicro- or millilensing) demagnifies it, but we cannot rule out thepossibility that SDSS J0924+0219 is an example of the relatively rareclass of ``three-component'' lens systems.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0304377</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Liebert, James</style></author><author><style face="normal" font="default" size="100%">Harris, H. C.</style></author><author><style face="normal" font="default" size="100%">Dahn, C. C.</style></author><author><style face="normal" font="default" size="100%">Schmidt, Gary D.</style></author><author><style face="normal" font="default" size="100%">Kleinman, S. J.</style></author><author><style face="normal" font="default" size="100%">Nitta, Atsuko</style></author><author><style face="normal" font="default" size="100%">Krzesiński, Jurek</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Szkody, Paula</style></author><author><style face="normal" font="default" size="100%">Hawley, Suzanne</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Collinge, Matthew J.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Margon, B.</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Silvestri, Nicole</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SDSS White Dwarfs with Spectra Showing Atomic Oxygen and/or Carbon Lines</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....126.2521L</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">126</style></volume><pages><style face="normal" font="default" size="100%">2521-2528</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We discuss 18 white dwarfs, one of which (G227-5) was previously known,whose SDSS spectra show lines of neutral and/or singly ionized carbon.At least two and perhaps four show lines of neutral or singly ionizedoxygen. Apart from the extremely hot ``PG 1159'' stars, these are thefirst white dwarfs with photospheric oxygen detected in their opticalspectra. The photometry strongly suggests that these stars lie in the11,000-30,000 K temperature range of the helium-atmosphere DB whitedwarfs, though only one of them shows weak neutral helium lines in thespectrum. Trigonometric parallaxes are known for G227-5 and another,previously known white dwarf (G35-26) showing atomic carbon lines, andthey indicate that both are massive stars. Theoretical arguments suggestthat all members of this class of rare white dwarfs are massive (~1M&lt;sub&gt;solar&lt;/sub&gt;), and this finding could explain the paucity ofmassive DB white dwarfs.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">DOI: 10.1086/378911</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Hall, Patrick B.</style></author><author><style face="normal" font="default" size="100%">Jester, Sebastian</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Brandt, W. N.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Gray, Jim</style></author><author><style face="normal" font="default" size="100%">Trump, Jonathan R.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Heckman, Timothy M.</style></author><author><style face="normal" font="default" size="100%">Hennessy, G. S.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Margon, Bruce</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Niederste-Ostholt, Martin</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Saxe, David H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Sloan Digital Sky Survey Quasar Catalog. II. First Data Release</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">December 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003AJ....126.2579S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">126</style></volume><pages><style face="normal" font="default" size="100%">2579-2593</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the second edition of the Sloan Digital Sky Survey (SDSS)Quasar Catalog. The catalog consists of the 16,713 objects in the SDSSFirst Data Release that have luminosities larger than M&lt;sub&gt;i&lt;/sub&gt;=-22(in a cosmology with H&lt;sub&gt;0&lt;/sub&gt;=70 km s&lt;sup&gt;-1&lt;/sup&gt;Mpc&lt;sup&gt;-1&lt;/sup&gt;, Ω&lt;sub&gt;M&lt;/sub&gt;=0.3, andΩ&lt;sub&gt;Λ&lt;/sub&gt;=0.7), have at least one emission line withFWHM larger than 1000 km s&lt;sup&gt;-1&lt;/sup&gt;, and have highly reliableredshifts. The area covered by the catalog is ~1360 deg&lt;sup&gt;2&lt;/sup&gt;. Thequasar redshifts range from 0.08 to 5.41, with a median value of 1.43.For each object, the catalog presents positions accurate to better than0.2&quot; rms per coordinate, five-band (ugriz) CCD-based photometry withtypical accuracy of 0.03 mag, and information on the morphology andselection method. The catalog also contains some radio, near-infrared,and X-ray emission properties of the quasars, when available, from otherlarge-area surveys. Calibrated digital spectra of all objects in thecatalog, covering the wavelength region 3800-9200 Å at a spectralresolution of 1800-2100, are available. This publication supersedes thefirst SDSS Quasar Catalog, which was based on material from the SDSSEarly Data Release. A summary of corrections to current quasar databasesis also provided. The majority of the objects were found in SDSScommissioning data using a multicolor selection technique. Since thequasar selection algorithm was undergoing testing during the entireobservational period covered by this catalog, care must be taken whenassembling samples from the catalog for use in statistical studies. A&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0308443</style></custom3><reprint-edition><style face="normal" font="default" size="100%">i=16.0 and 17 quasars with redshifts larger than 4.5.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Stanek, K. Z.</style></author><author><style face="normal" font="default" size="100%">Matheson, T.</style></author><author><style face="normal" font="default" size="100%">Garnavich, P. M.</style></author><author><style face="normal" font="default" size="100%">Martini, P.</style></author><author><style face="normal" font="default" size="100%">Berlind, P.</style></author><author><style face="normal" font="default" size="100%">Caldwell, N.</style></author><author><style face="normal" font="default" size="100%">Challis, P.</style></author><author><style face="normal" font="default" size="100%">Brown, W. R.</style></author><author><style face="normal" font="default" size="100%">Schild, R.</style></author><author><style face="normal" font="default" size="100%">Krisciunas, K.</style></author><author><style face="normal" font="default" size="100%">Calkins, M. L.</style></author><author><style face="normal" font="default" size="100%">Lee, J. C.</style></author><author><style face="normal" font="default" size="100%">Hathi, N.</style></author><author><style face="normal" font="default" size="100%">Jansen, R. A.</style></author><author><style face="normal" font="default" size="100%">Windhorst, R.</style></author><author><style face="normal" font="default" size="100%">Echevarria, L.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, D. J.</style></author><author><style face="normal" font="default" size="100%">Pindor, B.</style></author><author><style face="normal" font="default" size="100%">Olszewski, E. W.</style></author><author><style face="normal" font="default" size="100%">Harding, P.</style></author><author><style face="normal" font="default" size="100%">Holland, S. T.</style></author><author><style face="normal" font="default" size="100%">Bersier, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">July 1, 2003</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...591L..17S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">591</style></volume><pages><style face="normal" font="default" size="100%">L17-L20</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present early observations of the afterglow of GRB 030329 and thespectroscopic discovery of its associated supernova SN 2003dh. Weobtained spectra of the afterglow of GRB 030329 each night from March30.12 (0.6 days after the burst) to April 8.13 (UT) (9.6 days after theburst). The spectra cover a wavelength range of 350-850 nm. The earlyspectra consist of a power-law continuum(F&lt;sub&gt;ν&lt;/sub&gt;~ν&lt;sup&gt;-0.9&lt;/sup&gt;) with narrow emission linesoriginating from H II regions in the host galaxy, indicating a lowredshift of z=0.1687. However, our spectra taken after 2003 April 5 showbroad peaks in flux characteristic of a supernova. Correcting for theafterglow emission, we find that the spectrum of the supernova isremarkably similar to the Type Ic ``hypernova'' SN 1998bw. While thepresence of supernovae has been inferred from the light curves andcolors of gamma-ray burst afterglows in the past, this is the firstdirect, spectroscopic confirmation that a subset of classical gamma-raybursts originate from supernovae.Based on data from the Multiple Mirror Telescope Observatory 6.5 mtelescope, the Magellan 6.5 m Clay telescope, and the Fred LawrenceWhipple Observatory 1.5 m telescope.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0304173</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Schechter, Paul L.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Shimasaku, K.</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Velocity Dispersion Function of Early-Type Galaxies</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">September 1, 200</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2003ApJ...594..225S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">594</style></volume><pages><style face="normal" font="default" size="100%">225-231</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The distribution of early-type galaxy velocity dispersions,φ(σ), is measured using a sample drawn from the Sloan DigitalSky Survey database. Its shape differs significantly from that obtainedby simply using the mean correlation between luminosity L and velocitydispersion σ to transform the luminosity function into a velocityfunction: ignoring the scatter around the mean σ-L relation is abad approximation. An estimate of the contribution from late-typegalaxies is also made, which suggests that φ(σ) is dominatedby early-type galaxies at velocities larger than ~200 km s&lt;sup&gt;-1&lt;/sup&gt;.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0303092</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andy</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Narayanan, Vijay</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Liam</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkman, Jon</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert</style></author><author><style face="normal" font="default" size="100%">Ivezic, Zeljko</style></author><author><style face="normal" font="default" size="100%">Kim, Rita S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy</style></author><author><style face="normal" font="default" size="100%">Munn, Jeff</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeff</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Analysis of Systematic Effects and Statistical Uncertainties in Angular Clustering of Galaxies from Early Sloan Digital Sky Survey Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2002</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2002</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2002ApJ...579...48S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">579</style></volume><pages><style face="normal" font="default" size="100%">48-75</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The angular distribution of galaxies encodes a wealth of informationabout large-scale structure. Ultimately, the Sloan Digital Sky Survey(SDSS) will record the angular positions of order of 10&lt;sup&gt;8&lt;/sup&gt;galaxies in five bands, adding significantly to the cosmologicalconstraints. This is the first in a series of papers analyzing arectangular stripe of 2.5d×90&lt;sup&gt;deg&lt;/sup&gt; from early SDSS data.We present the angular correlation function for galaxies in fourseparate magnitude bins on angular scales ranging from 0.003d to15°. Much of the focus of this paper is on potential systematiceffects. We show that the final galaxy catalog-with the mask accountingfor regions of poor seeing, reddening, bright stars, etc.-is free fromexternal and internal systematic effects for galaxies brighter thanr&lt;sup&gt;*&lt;/sup&gt;=22. Our estimator of the angular correlation functionincludes the effects of the integral constraint and the mask. The fullcovariance matrix of errors in these estimates is derived using mockcatalogs with further estimates using a number of other methods. Basedon observations obtained with the Sloan Digital Sky Survey.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0107416</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Liam</style></author><author><style face="normal" font="default" size="100%">Postman, Marc</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Hennessy, G. S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert</style></author><author><style face="normal" font="default" size="100%">Ichikawa, Takashi</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kim, Rita S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter</style></author><author><style face="normal" font="default" size="100%">Lamb, D. Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeff</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeff</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Angular Correlation Function of Galaxies from Early Sloan Digital Sky Survey Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2002</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2002</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2002ApJ...579...42C</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">579</style></volume><pages><style face="normal" font="default" size="100%">42-47</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;The Sloan Digital Sky Survey is one of the first multicolor photometricand spectroscopic surveys designed to measure the statistical propertiesof galaxies within the local universe. In this paper we present some ofthe initial results on the angular two-point correlation functionmeasured from the early SDSS galaxy data. The form of the correlationfunction, over the magnitude interval 18*&amp;lt;22, isshown to be consistent with results from existing wide-field,photographic-based surveys and narrower CCD galaxy surveys. On scalesbetween 1' and 1° the correlation function is well described by apower law with an exponent of ~-0.7. The amplitude of the correlationfunction, within this angular interval, decreases with faintermagnitudes in good agreement with analysis from existing galaxy surveys.There is a characteristic break in the correlation function on scales ofapproximately 1°-2°. On small scales, θ&amp;lt;1&lt;sup&gt;'&lt;/sup&gt;,the SDSS correlation function does not appear to be consistent with thepower-law form fitted to the 1&lt;sup&gt;'&lt;/sup&gt;&amp;lt;θ&amp;lt;0.5d data.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0107417</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Narayanan, Vijay</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hui, Lam</style></author><author><style face="normal" font="default" size="100%">Jain, Bhuvnesh</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">O'Connell, Liam</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Hennessy, Greg</style></author><author><style face="normal" font="default" size="100%">Ivezíc, Željko</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The Angular Power Spectrum of Galaxies from Early Sloan Digital Sky Survey Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2002</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2002</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2002ApJ...571..191T</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">571</style></volume><pages><style face="normal" font="default" size="100%">191-205</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We compute the angular power spectrum C&lt;sub&gt;l&lt;/sub&gt; from 1.5 milliongalaxies in early Sloan Digital Sky Survey (SDSS) data on large angularscales, l&amp;lt;~600. The data set covers about 160 deg&lt;sup&gt;2&lt;/sup&gt;, with acharacteristic depth on the order of 1 h&lt;sup&gt;-1&lt;/sup&gt; Gpc in thefaintest (21*&amp;lt;22) of our four magnitude bins.Cosmological interpretations of these results are presented in acompanion paper by Dodelson and coworkers. The data in all fourmagnitude bins are consistent with a simple flat ``concordance'' modelwith nonlinear evolution and linear bias factors on the order of unity.Nonlinear evolution is particularly evident for the brightest galaxies.A series of tests suggests that systematic errors related to seeing,reddening, etc. are negligible, which bodes well for the 60-fold largersample that the SDSS is currently collecting. Uncorrelated error barsand well-behaved window functions make our measurements a convenientstarting point for cosmological model fitting.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0107418</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Zehavi, Idit</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Weinberg, David H.</style></author><author><style face="normal" font="default" size="100%">Mo, Houjun J.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Briggs, John W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jon</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Carey, Larry</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Csabai, Istvan</style></author><author><style face="normal" font="default" size="100%">Dalcanton, Julianne J.</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Evans, Michael L.</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas P.</style></author><author><style face="normal" font="default" size="100%">Friedman, Scott</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hennessy, Greg S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Kron, Richard</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter</style></author><author><style face="normal" font="default" size="100%">Lamb, Donald Q.</style></author><author><style face="normal" font="default" size="100%">Leger, R. French</style></author><author><style face="normal" font="default" size="100%">Long, Daniel C.</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Merrelli, Aronne</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Narayanan, Vijay</style></author><author><style face="normal" font="default" size="100%">Newcomb, Matt</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Owen, Russell</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pope, Adrian</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Sheth, Ravi K.</style></author><author><style face="normal" font="default" size="100%">Siegmund, Walter</style></author><author><style face="normal" font="default" size="100%">Smee, Stephen</style></author><author><style face="normal" font="default" size="100%">Snir, Yehuda</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Szapudi, Istvan</style></author><author><style face="normal" font="default" size="100%">Tegmark, Max</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Uomoto, Alan</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Dan</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Waddell, Patrick</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Galaxy Clustering in Early Sloan Digital Sky Survey Redshift Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2002</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2002</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2002ApJ...571..172Z</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">571</style></volume><pages><style face="normal" font="default" size="100%">172-190</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present the first measurements of clustering in the Sloan Digital SkySurvey (SDSS) galaxy redshift survey. Our sample consists of 29,300galaxies with redshifts5700kms&lt;sup&gt;-1&lt;/sup&gt;&amp;lt;=cz&amp;lt;=39,000kms&lt;sup&gt;-1&lt;/sup&gt;, distributed inseveral long but narrow (2.5d-5°) segments, covering 690deg&lt;sup&gt;2&lt;/sup&gt;. For the full, flux-limited sample, the redshift-spacecorrelation length is approximately 8 h&lt;sup&gt;-1&lt;/sup&gt; Mpc. Thetwo-dimensional correlation function ξ(r&lt;sub&gt;p&lt;/sub&gt;,π) showsclear signatures of both the small-scale, ``fingers-of-God'' distortioncaused by velocity dispersions in collapsed objects and the large-scalecompression caused by coherent flows, though the latter cannot bemeasured with high precision in the present sample. The inferredreal-space correlation function is well described by a power law,ξ(r)=(r/6.1+/-0.2h&lt;sup&gt;-1&lt;/sup&gt;Mpc)&lt;sup&gt;-1.75+/-0.03&lt;/sup&gt;, for0.1h&lt;sup&gt;-1&lt;/sup&gt;Mpc&amp;lt;=r&amp;lt;=16h&lt;sup&gt;-1&lt;/sup&gt;Mpc. The galaxy pairwisevelocity dispersion is σ&lt;sub&gt;12&lt;/sub&gt;~600+/-100kms&lt;sup&gt;-1&lt;/sup&gt;for projected separations0.15h&lt;sup&gt;-1&lt;/sup&gt;Mpc&amp;lt;=r&lt;sub&gt;p&lt;/sub&gt;&amp;lt;=5h&lt;sup&gt;-1&lt;/sup&gt;Mpc. When wedivide the sample by color, the red galaxies exhibit a stronger andsteeper real-space correlation function and a higher pairwise velocitydispersion than do the blue galaxies. The relative behavior ofsubsamples defined by high/low profile concentration or high/low surfacebrightness is qualitatively similar to that of the red/blue subsamples.Our most striking result is a clear measurement of scale-independentluminosity bias at r&amp;lt;~10h&lt;sup&gt;-1&lt;/sup&gt;Mpc: subsamples with absolutemagnitude ranges centered on M&lt;sub&gt;*&lt;/sub&gt;-1.5, M&lt;sub&gt;*&lt;/sub&gt;, andM&lt;sub&gt;*&lt;/sub&gt;+1.5 have real-space correlation functions that areparallel power laws of slope ~-1.8 with correlation lengths ofapproximately 7.4, 6.3, and 4.7 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, respectively.&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0106476</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Szapudi, István</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Scoccimarro, Roman</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Connolly, Andrew J.</style></author><author><style face="normal" font="default" size="100%">Dodelson, Scott</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Johnston, David</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Loveday, Jon</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">Scranton, Ryan</style></author><author><style face="normal" font="default" size="100%">Stebbins, Albert</style></author><author><style face="normal" font="default" size="100%">Vogeley, Michael S.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Brinkman, J.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kim, Rita S. J.</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Lamb, Don Q.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">McKay, Timothy A.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeff</style></author><author><style face="normal" font="default" size="100%">Peoples, John</style></author><author><style face="normal" font="default" size="100%">Pier, Jeff</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Stoughton, Christopher</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">York, Douglas G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Higher Order Moments of the Angular Distribution of Galaxies from Early Sloan Digital Sky Survey Data</style></title><secondary-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2002</style></year><pub-dates><date><style  face="normal" font="default" size="100%">May 1, 2002</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2002ApJ...570...75S</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">570</style></volume><pages><style face="normal" font="default" size="100%">75-85</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We present initial results for counts in cell statistics of the angulardistribution of galaxies in early data from the Sloan Digital Sky Survey(SDSS). We analyze a rectangular stripe 2.5d wide, coveringapproximately 160 deg&lt;sup&gt;2&lt;/sup&gt;, containing over 10&lt;sup&gt;6&lt;/sup&gt;galaxies in the apparent magnitude range 18'&amp;lt;22, withareas of bad seeing, contamination from bright stars, ghosts, and highgalactic extinction masked out. This survey region, which forms part ofthe SDSS early data release, is the same as that for which two-pointangular clustering statistics have recently been computed. The third andfourth moments of the cell counts, s&lt;sub&gt;3&lt;/sub&gt; (skewness) ands&lt;sub&gt;4&lt;/sub&gt; (kurtosis), constitute the most accurate measurements todate of these quantities (for r&lt;sup&gt;'&lt;/sup&gt;&amp;lt;21) over angular scales0.015d-0.3d. They display the approximate hierarchical scaling expectedfrom nonlinear structure formation models and are in reasonableagreement with the predictions of Λ-dominated cold dark mattermodels with galaxy biasing that suppresses higher order correlations atsmall scales. The results are, in general, consistent with previousmeasurements in the APM, EDSGC, and Deeprange surveys. These resultssuggest that the SDSS imaging data are free of systematics to a highdegree and will therefore enable determination of the skewness and&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0111058</style></custom3></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Menou, Kristen</style></author><author><style face="normal" font="default" size="100%">Knapp, Gillian R.</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Tremonti, Christy</style></author><author><style face="normal" font="default" size="100%">Weinstein, Michael A.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Becker, Robert H.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel</style></author><author><style face="normal" font="default" size="100%">Fan, Xiaohui</style></author><author><style face="normal" font="default" size="100%">Finkbeiner, Douglas</style></author><author><style face="normal" font="default" size="100%">Finlator, Kristian</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua</style></author><author><style face="normal" font="default" size="100%">Gunn, James E.</style></author><author><style face="normal" font="default" size="100%">Hall, Pat B.</style></author><author><style face="normal" font="default" size="100%">Kim, Rita S. J.</style></author><author><style face="normal" font="default" size="100%">Kinkhabwala, Ali</style></author><author><style face="normal" font="default" size="100%">Narayanan, Vijay K.</style></author><author><style face="normal" font="default" size="100%">Rockosi, Constance M.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David</style></author><author><style face="normal" font="default" size="100%">Schneider, Donald P.</style></author><author><style face="normal" font="default" size="100%">Strateva, Iskra</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Wolfgang Voges</style></author><author><style face="normal" font="default" size="100%">White, Richard L.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Brinkmann, Jonathan</style></author><author><style face="normal" font="default" size="100%">Doi, Mamoru</style></author><author><style face="normal" font="default" size="100%">Fukugita, Masataka</style></author><author><style face="normal" font="default" size="100%">Hennessy, Gregory S.</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Nichol, Robert C.</style></author><author><style face="normal" font="default" size="100%">York, Donald G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Optical and Radio Properties of Extragalactic Sources Observed by the FIRST Survey and the Sloan Digital Sky Survey</style></title><secondary-title><style face="normal" font="default" size="100%">The Astronomical Journal</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2002</style></year><pub-dates><date><style  face="normal" font="default" size="100%">November 1, 2002</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">http://adsabs.harvard.edu/abs/2002AJ....124.2364I</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">124</style></volume><pages><style face="normal" font="default" size="100%">2364-2400</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">&lt;p&gt;We discuss the optical and radio properties of ~30,000 FIRST (radio, 20cm, sensitive to 1 mJy) sources positionally associated within 1.5&quot; witha Sloan Digital Sky Survey (SDSS) (optical, sensitive to r*~22.2) source&lt;/p&gt;
</style></abstract><notes><style face="normal" font="default" size="100%">n/a</style></notes><custom3><style face="normal" font="default" size="100%">eprintid: arXiv:astro-ph/0202408</style></custom3><reprint-edition><style face="normal" font="default" size="100%">emission from starburst galaxies.</style></reprint-edition></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Stoughton, Chris</style></author><author><style face="normal" font="default" size="100%">Lupton, Robert H.</style></author><author><style face="normal" font="default" size="100%">Bernardi, Mariangela</style></author><author><style face="normal" font="default" size="100%">Blanton, Michael R.</style></author><author><style face="normal" font="default" size="100%">Burles, Scott</style></author><author><style face="normal" font="default" size="100%">Castander, Francisco J.</style></author><author><style face="normal" font="default" size="100%">Connolly, A. J.</style></author><author><style face="normal" font="default" size="100%">Eisenstein, Daniel J.</style></author><author><style face="normal" font="default" size="100%">Frieman, Joshua A.</style></author><author><style face="normal" font="default" size="100%">Hennessy, G. S.</style></author><author><style face="normal" font="default" size="100%">Hindsley, Robert B.</style></author><author><style face="normal" font="default" size="100%">Ivezić, Željko</style></author><author><style face="normal" font="default" size="100%">Kent, Stephen</style></author><author><style face="normal" font="default" size="100%">Kunszt, Peter Z.</style></author><author><style face="normal" font="default" size="100%">Lee, Brian C.</style></author><author><style face="normal" font="default" size="100%">Meiksin, Avery</style></author><author><style face="normal" font="default" size="100%">Munn, Jeffrey A.</style></author><author><style face="normal" font="default" size="100%">Newberg, Heidi Jo</style></author><author><style face="normal" font="default" size="100%">Nichol, R. C.</style></author><author><style face="normal" font="default" size="100%">Nicinski, Tom</style></author><author><style face="normal" font="default" size="100%">Pier, Jeffrey R.</style></author><author><style face="normal" font="default" size="100%">Richards, Gordon T.</style></author><author><style face="normal" font="default" size="100%">Richmond, Michael W.</style></author><author><style face="normal" font="default" size="100%">Schlegel, David J.</style></author><author><style face="normal" font="default" size="100%">Smith, J. Allyn</style></author><author><style face="normal" font="default" size="100%">Strauss, Michael A.</style></author><author><style face="normal" font="default" size="100%">SubbaRao, Mark</style></author><author><style face="normal" font="default" size="100%">Szalay, Alexander S.</style></author><author><style face="normal" font="default" size="100%">Thakar, Aniruddha R.</style></author><author><style face="normal" font="default" size="100%">Tucker, Douglas L.</style></author><author><style face="normal" font="default" size="100%">Vanden Berk, Daniel E.</style></author><author><style face="normal" font="default" size="100%">Yanny, Brian</style></author><author><style face="normal" font="default" size="100%">Adelman, Jennifer K.</style></author><author><style face="normal" font="default" size="100%">Anderson, John E., Jr.</style></author><author><style face="normal" font="default" size="100%">Anderson, Scott F.</style></author><author><style face="normal" font="default" size="100%">Annis, James</style></author><author><style face="normal" font="default" size="100%">Bahcall, Neta A.</style></author><author><style face="normal" font="default" size="100%">Bakken, J. A.</style></author><author><style face="normal" font="default" size="100%">Bartelmann, Matthias</style></author><author><style face="normal" font="default" size="100%">Bastian, Steven</style></author><author><style face="normal" font="default" size="100%">Bauer, Amanda</style></author><author><style face="normal" font="default" size="100%">Berman, Eileen</style></author><author><style face="normal" font="default" size="100%">Böhringer, Hans</style></author><author><style face="normal" font="default" size="100%">Boroski, William N.</style></author><author><style face="normal" font="default" size="100%">Bracker, Steve</style></author><author><style face="normal" font="default" size="100%">Briegel, Charlie</style></author><author><style face="normal" font="default" size="100%">Briggs, John W.</style></author><author><style face="normal" font="default" size="100%">Brinkmann, J.</style></author><author><style face="normal" font="default" size="100%">Brunner, Robert</style></author><author><style face="normal" font="default" size="100%">Carey, Larry</style></author><author><style face="normal" font="default" size="100%">Carr, Michael A.</style></author><author><style face="normal" font="default" size="100%">Chen, Bing</style></author><author><style face="normal" font="default" size="100%">Christian, Damian</style></author><author><style face="normal" font="default" size="100%">Colestock, Patrick L.</style></author><author><style face="normal" font="default" size="100%">Crocker, J. H.</style></author><author><style face="normal" font="default" size="100%">Csabai, István</style></author><author><style face="normal" font="default" size="100%">Czarapata, Paul C.</style></author><author><style face="normal" font="default" size="100%">Dalcanton, Julianne</style></author><author><style face="normal" font="default" size="100%">Davidsen, Arthur F.</style></author><author><style face="normal" font="default" size="100%">Davis, John Eric</style></author><author><style face="normal" font="default" size="100%">Dehnen, Walter</style></author><author><style face=