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26 April 2024

» arxiv » astro-ph/0107421

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The 3D Power Spectrum from Angular Clustering of Galaxies in Early SDSS Data
Scott Dodelson ; Vijay K. Narayanan ; Max Tegmark ; Ryan Scranton ; Tamas Budavari ; Andrew Connolly ; Istvan Csabai ; Daniel Eisenstein ; Joshua A. Frieman ; James E. Gunn ; Lam Hui ; Bhuvnesh Jain ; David Johnston ; Stephen Kent ; Jon Loveday ; Robert C. Nichol ; Liam O’Connell ; Roman Scoccimarro ; Ravi K. Sheth ; Albert Stebbins ; Michael A. Strauss ; Alexander S. Szalay ; István Szapudi ; Michael S. Vogeley ; Idit Zehavi ; et al ; for the SDSS Collaboration ;
Date:	20 Jul 2001
Journal:	Astrophys.J. 572 (2001) 140-156
Subject:	astro-ph
Abstract:	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 $w( heta)$ and 2D power spectrum $C_l$ of these galaxies are presented. Here we invert Limber’s equation to extract the 3D 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 3D power spectrum estimates from $w( heta)$ and $C_l$ agree with each other and with previous estimates over a range in wavenumbers $0.03 < k/{ m h Mpc}^{-1} < 1$. The galaxies in the faintest magnitude bin ($21 < star < 22$, which have median redshift $z_m=0.43$) are less clustered than the galaxies in the brightest magnitude bin ($18 < star < 19$ with $z_m=0.17$), especially on scales where nonlinearities are important. The derived power spectrum agrees with that of Szalay et al. (2001) who go directly from the raw data to a parametric estimate of the power spectrum. The strongest constraints on the shape parameter $Gamma$ come from the faintest galaxies (in the magnitude bin $21 < star < 22$), from which we infer $Gamma = 0.14^{+0.11}_{-0.06}$ (95% C.L.).
Source:	arXiv, astro-ph/0107421
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