Max Tegmark, Massachusetts Institute of Technology
Daniel J. Eisenstein, University of Arizona
Michael Strauss, Princeton University Observatory
David H. Weinberg, Ohio State University
Michael R. Blanton, New York University
Joshua A. Frieman, University of Chicago
Masataka Fukugita, University of Tokyo
James E. Gunn, Princeton University Observatory
Andrew J. S. Hamilton, University of Colorado, Boulder
Gillian R. Knapp, Princeton University Observatory
Robert C. Nichol, University of Portsmouth
Jeremiah P. Ostriker, Princeton University Observatory
Nikhil Padmanabhan, Princeton University
Will J. Percival, University of Portsmouth
David J. Schlegel, Lawrence Berkeley National Laboratory
Donald P. Schneider, The Pennsylvania State University
Roman Scoccimarro, New York University
Uroš Seljak, Princeton University
Hee-Jong Seo, University of Arizona
Molly Swanson, Massachusetts Institute of Technology
Alexander S. Szalay, The Johns Hopkins University
Michael S. Vogeley, Drexel University
Jaiyul Yoo, Ohio State University
Idit Zehavi, Case Western Reserve University
Kevork Abazajian, Los Alamos National Laboratory
Scott F. Anderson, University of Washington
James Annis, Fermi National Accelerator Laboratory
Neta A. Bahcall, Princeton University Observatory
Bruce Bassett, South African Astronomical Observatory
Andreas Berlind, New York University
John Brinkman, Apache Point Observatory
Tamás Budavari, The Johns Hopkins University
Francisco Castander, Institut d’Estudis Espacials de Catalunya/CSIC
Andrew Connolly, University of Pittsburgh
Istvan Csabai, The Johns Hopkins University
Mamoru Doi, University of Tokyo
Douglas P. Finkbeiner, Princeton University Observatory
Bruce Gillespie, Apache Point Observatory
Karl Glazebrook, The Johns Hopkins University
Gregory S. Hennessy, U.S. Naval Observatory
David W. Hogg, New York University
Željko Ivezić, Princeton University Observatory
Bhuvnesh Jain, University of Pennsylvania
David Johnston, Jet Propulsion Laboratory
Stephen Kent, Fermi National Accelerator Laboratory
Donald Q. Lamb, University of Chicago
Brian C. Lee, Lawrence Berkeley National Laboratory
Huan Lin, Fermi National Accelerator Laboratory
Jon Loveday, University of Sussex
Robert H. Lupton, Princeton University Observatory
Jeffrey A. Munn, U.S. Naval Observatory
Kaike Pan, Apache Point Observatory
Changbom Park, Seoul National University
John Peoples, Fermi National Accelerator Laboratory
Jeffrey R. Pier, U.S. Naval Observatory
Adrian Pope, The Johns Hopkins University
Michael Richmond, Rochester Institute of TechnologyFollow
Constance Rockosi, University of Chicago
Ryan Scranton, University of Pittsburgh
Ravi K. Sheth, University of Pennsylvania
Albert Stebbins, Fermi National Accelerator Laboratory
Christopher Stoughton, Fermi National Accelerator Laboratory
István Szapudi, University of Hawaii, Honolulu
Douglas L. Tucker, Fermi National Accelerator Laboratory
Daniel E. Vanden Berk, University of Pittsburgh
Brian Yanny, Fermi National Accelerator Laboratory
Donald G. York, University of Chicago


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-Lo`eve 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 0.01 h/Mpc < k < 0.2 h/Mpc. Results from the LRG and main galaxy samples are consistent, with the former providing higher signal-to-noise. Our results are robust to omitting angular and radial density fluctuations and are consistent between different parts of the sky. They provide a striking confirmation of the predicted large-scale CDM power spectrum. Combining only SDSS LRG and WMAP data places robust constraints on many cosmological parameters that complement prior analyses of multiple data sets. The LRGs provide independent cross-checks on m and the baryon fraction in good agreement with WMAP. Within the context of flat CDM models, our LRG measurements complementWMAP by sharpening the constraints on the matter density, the neutrino density and the tensor amplitude by about a factor of two, giving m = 0.24±0.02 (1 ), Pmν < 0.9 eV (95%) and r < 0.3 (95%). Baryon oscillations are clearly detected and provide a robust measurement of the comoving distance to the median survey redshift z = 0.35 independent of curvature and dark energy properties. Within the CDM framework, our power spectrum measurement improves the evidence for spatial flatness, sharpening the curvature constraint tot = 1.05±0.05 from WMAP alone to tot = 1.003±0.010. Assuming tot = 1, the equation of state parameter is constrained to w = −0.94±0.09, indicating the potential for more ambitious future LRG measurements to provide precision tests of the nature of dark energy. All these constraints are essentially independent of scales k > 0.1h/Mpc and associated nonlinear complications, yet agree well with more aggressive published analyses where nonlinear modeling is crucial.

Publication Date



This is a pre-print of an article published by the American Physical Society. ©2006 American Physical Society. The final, published version is located here:

Also archived in: arXiv:astro-ph/0608632 v2 Oct 30 2006

Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type


Department, Program, or Center

School of Physics and Astronomy (COS)


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