Cosmological constraints from the SDSS luminous red galaxies
Max Tegmark,Daniel J. Eisenstein,Michael A. Strauss,David H. Weinberg,Michael R. Blanton,Joshua A. Frieman,Joshua A. Frieman,Masataka Fukugita,James E. Gunn,Andrew J. S. Hamilton,Gillian R. Knapp,Robert C. Nichol,Jeremiah P. Ostriker,Nikhil Padmanabhan,Will J. Percival,David J. Schlegel,Donald P. Schneider,Roman Scoccimarro,Uroš Seljak,Uroš Seljak,Hee-Jong Seo,Molly E. C. Swanson,Alexander S. Szalay,Michael S. Vogeley,Jaiyul Yoo,Idit Zehavi,Kevork N. Abazajian,Scott F. Anderson,James Annis,Neta A. Bahcall,Bruce A. Bassett,Andreas A. Berlind,Jon Brinkmann,Tamás Budavári,Francisco J. Castander,Andrew J. Connolly,István Csabai,Mamoru Doi,Douglas P. Finkbeiner,Douglas P. Finkbeiner,Bruce Gillespie,Karl Glazebrook,Gregory S. Hennessy,David W. Hogg,Željko Ivezić,Željko Ivezić,Bhuvnesh Jain,David Johnston,Stephen M. Kent,D. Q. Lamb,Brian C. Lee,Huan Lin,Jon Loveday,Robert H. Lupton,Jeffrey A. Munn,Kaike Pan,Changbom Park,John Peoples,Jeffrey R. Pier,Adrian Pope,Michael Richmond,Constance M. Rockosi,Ryan Scranton,Ravi K. Sheth,Albert Stebbins,Christopher Stoughton,István Szapudi,Douglas L. Tucker,Daniel E. Vanden Berk,Brian Yanny,Donald G. York +70 more
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In this paper, the authors employed a matrix-based power spectrum estimation method using pseudo-Karhunen-Loeve eigenmodes, producing uncorrelated minimum-variance measurements in 20 k-bands of both the clustering power and its anisotropy due to redshift-space distortions.Abstract:
We measure the large-scale real-space power spectrum P(k) using luminous red galaxies (LRGs) in the Sloan Digital Sky Survey (SDSS) and use this measurement to sharpen constraints on cosmological parameters from the Wilkinson Microwave Anisotropy Probe (WMAP). We employ a matrix-based power spectrum estimation method using Pseudo-Karhunen-Loeve eigenmodes, producing uncorrelated minimum-variance measurements in 20 k-bands of both the clustering power and its anisotropy due to redshift-space distortions, with narrow and well-behaved window functions in the range 0.01h/Mpc 0.1h/Mpc and associated nonlinear complications, yet agree well with more aggressive published analyses where nonlinear modeling is crucial.read more
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