Journal
ASTROPHYSICAL JOURNAL
Volume 572, Issue 1, Pages 140-156Publisher
IOP Publishing Ltd
DOI: 10.1086/340225
Keywords
galaxies : clusters : general; galaxies : statistics
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Early photometric data from the Sloan Digital Sky Survey (SDSS) contain angular positions for 1.5 million galaxies. In companion papers, the angular correlation function w(theta) and two-dimensional power spectrum Cl of these galaxies are presented. Here we invert Limbers equation to extract the three-dimensional power spectrum from the angular results. We accomplish this using an estimate of dn/dz, the redshift distribution of galaxies in four different magnitude slices in the SDSS photometric catalog. The resulting three-dimensional power spectrum estimates from w(theta) and C-l agree with each other and with previous estimates over a range in wavenumbers 0.03 < k/ (h Mpc(-1)) < 1. The galaxies in the faintest magnitude bin (21 < r* < 22, which have median redshift z(m) = 0.43) are less clustered than the galaxies in the brightest magnitude bin (18 < r* < 19 with z(m) = 0.17), especially on scales where nonlinearities are important. The derived power spectrum agrees with that of Szalay et al., who go directly from the raw data to a parametric estimate of the power spectrum. The strongest constraints on the shape parameter C come from the faintest galaxies (in the magnitude bin 21 < r* < 22), from which we infer Gamma = 0.14(-0.06)(+0.11) (95% CL).
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