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