<?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%">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></records></xml>