Citation:
Date Published:
June 1, 2002Abstract:
Early photometric data from the Sloan Digital Sky Survey (SDSS) containangular positions for 1.5 million galaxies. In companion papers, theangular correlation function w(θ) and two-dimensional powerspectrum Cl of these galaxies are presented. Here we invertLimber's equation to extract the three-dimensional power spectrum fromthe angular results. We accomplish this using an estimate of dn/dz, theredshift distribution of galaxies in four different magnitude slices inthe SDSS photometric catalog. The resulting three-dimensional powerspectrum estimates from w(θ) and Cl agree with eachother and with previous estimates over a range in wavenumbers0.03-1)<1. The galaxies in the faintestmagnitude bin (21*<22, which have median redshiftzm=0.43) are less clustered than the galaxies in thebrightest magnitude bin (18*<19 withzm=0.17), especially on scales where nonlinearities areimportant. The derived power spectrum agrees with that of Szalay et al.,who go directly from the raw data to a parametric estimate of the powerspectrum. The strongest constraints on the shape parameter Γ comefrom the faintest galaxies (in the magnitude bin21*<22), from which we infer