%0 Journal Article %J The Astrophysical Journal %D 2002 %T The Three-dimensional Power Spectrum from Angular Clustering of Galaxies in Early Sloan Digital Sky Survey Data %A Dodelson, Scott %A Narayanan, Vijay K. %A Tegmark, Max %A Scranton, Ryan %A Budavári, Tamas %A Connolly, Andrew %A Csabai, Istvan %A Eisenstein, Daniel %A Frieman, Joshua A. %A Gunn, James E. %A Hui, Lam %A Jain, Bhuvnesh %A Johnston, David %A Kent, Stephen %A Loveday, Jon %A Nichol, Robert C. %A O'Connell, Liam %A Scoccimarro, Roman %A Sheth, Ravi K. %A Stebbins, Albert %A Strauss, Michael A. %A Szalay, Alexander S. %A Szapudi, István %A Vogeley, Michael S. %A Zehavi, Idit %A Annis, James %A Bahcall, Neta A. %A Brinkman, Jon %A Doi, Mamoru %A Fukugita, Masataka %A Hennessy, Greg %A Ivezić, Željko %A Knapp, Gillian R. %A Kunszt, Peter %A Lamb, Don Q. %A Lee, Brian C. %A Lupton, Robert H. %A Munn, Jeffrey A. %A Peoples, John %A Pier, Jeffrey R. %A Rockosi, Constance %A Schlegel, David %A Stoughton, Christopher %A Tucker, Douglas L. %A Yanny, Brian %A York, Donald G. %X

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

%B The Astrophysical Journal %V 572 %P 140-156 %8 June 1, 2002 %G eng %U http://adsabs.harvard.edu/abs/2002ApJ...572..140D %3 eprintid: arXiv:astro-ph/0107421