Measuring the baryon acoustic oscillation scale using the sloan digital sky survey and 2dF galaxy redshift survey

被引:675
作者
Percival, Will J. [1 ]
Cole, Shaun
Eisenstein, Daniel J.
Nichol, Robert C.
Peacock, John A.
Pope, Adrian C.
Szalay, Alexander S.
机构
[1] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 2EG, Hants, England
[2] Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England
[3] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA
[4] Univ Edinburgh, Astron Inst, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland
[5] Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA
[6] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
基金
英国科学技术设施理事会;
关键词
cosmology : observations; distance scale; large-scale structure of Universe;
D O I
10.1111/j.1365-2966.2007.12268.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We introduce a method to constrain general cosmological models using Baryon Acoustic Oscillation ( BAO) distance measurements from galaxy samples covering different redshift ranges, and apply this method to analyse samples drawn from the Sloan Digital Sky Survey ( SDSS) and 2dF Galaxy Redshift Survey ( 2dFGRS). BAOs are detected in the clustering of the combined 2dFGRS and SDSS main galaxy samples, and measure the distance - redshift relation at z = 0.2. BAOs in the clustering of the SDSS luminous red galaxies measure the distance - redshift relation at z = 0.35. The observed scales of the BAOs calculated from these samples and from the combined sample are jointly analysed using estimates of the correlated errors, to constrain the form of the distance measure D-V( z)=[( 1+ z)(2)D(A)(2)cz/H(z)](1/ 3). Here D-A is the angular diameter distance, and H( z) is the Hubble parameter. This gives r(s)/ DV( 0.2) = 0.1980 +/- 0.0058 and r(s)/ DV( 0.35)= 0.1094 +/- 0.0033 ( 1s errors), with a correlation coefficient of 0.39, where r(s) is the comoving sound horizon scale at recombination. Matching the BAOs to have the same measured scale at all redshifts then gives DV( 0.35)/ DV( 0.2) = 1.812 0.060. The recovered ratio is roughly consistent with that predicted by the higher redshift Supernova Legacy Survey ( SNLS) supernova data for Lambda cold dark matter cosmologies, but does require slightly stronger cosmological acceleration at a low redshift. If we force the cosmological model to be flat with constant w, then we find ohm(m) = 0.249 +/- 0.018 and w =- 1.004 +/- 0.089 after combining with the SNLS data, and including the WMAP measurement of the apparent acoustic horizon angle in the cosmic microwave background.
引用
收藏
页码:1053 / 1066
页数:14
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