Tegmark, Max and Eisenstein, Daniel J. and Strauss, Michael A. and Weinberg, David H. and Blanton, Michael R. and Frieman, Joshua A. and Fukugita, Masataka and Gunn, James E. and Hamilton, Andrew J. S. and Knapp, Gillian R. and Nichol, Robert C. and Ostriker, Jeremiah P. and Padmanabhan, Nikhil and Percival, Will J. and Schlegel, David J. and Schneider, Donald P. and Scoccimarro, Roman and Seljak, Uroš and Seo, Hee-Jong and Swanson, Molly and Szalay, Alexander S. and Vogeley, Michael S. and Yoo, Jaiyul and Zehavi, Idit and Abazajian, Kevork and Anderson, Scott F. and Annis, James and Bahcall, Neta A. and Bassett, Bruce and Berlind, Andreas and Brinkmann, Jon and Budavari, Tamás and Castander, Francisco and Connolly, Andrew and Csabai, Istvan and Doi, Mamoru and Finkbeiner, Douglas P. and Gillespie, Bruce and Glazebrook, Karl and Hennessey, Gregory S. and Hogg, David W. and Ivezić, Željko and Jain, Bhuvnesh and Johnston, David and Kent, Stephen and Lamb, Donald Q. and Lee, Brian C. and Lin, Huan and Loveday, Jon and Lupton, Robert H. and Munn, Jeffrey A. and Park, Changbom and Peoples, John and Pier, Jeffrey R. and Pope, Adrian and Richmond, Michael and Rockosi, Constance and Scranton, Ryan and Sheth, Ravi K. and Stebbins, Albert and Stoughton, Christopher and Szapudi, István and Tucker, Douglas L. and Vanden Berk, Daniel E. and Yanny, Brian and York, Donald G. (2006) Cosmological constraints from the SDSS luminous red galaxies. Physical Review D, 74 (12). Art. No. 123507. ISSN 0556-2821 http://resolver.caltech.edu/CaltechAUTHORS:TEGprd06
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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-Loève 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<k<0.2h/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 LambdaCDM 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 Omegam and the baryon fraction in good agreement with WMAP. Within the context of flat LambdaCDM models, our LRG measurements complement WMAP by sharpening the constraints on the matter density, the neutrino density and the tensor amplitude by about a factor of 2, giving Omegam=0.24±0.02 (1sigma), (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 LambdaCDM framework, our power spectrum measurement improves the evidence for spatial flatness, sharpening the curvature constraint Omegatot=1.05±0.05 from WMAP alone to Omegatot=1.003±0.010. Assuming Omegatot=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.
|Additional Information:||©2006 The American Physical Society. (Received 22 August 2006; published 11 December 2006) We thank Angelica de Oliveira-Costa, Kirsten A. Hubbard, Oliver Zahn, and Matias Zaldarriaga for helpful comments, and Dulce Gonçalves de Oliveira-Costa for ground support. We thank the WMAP team for making data and Monte Carlo Markov chains public via the Legacy Archive for Microwave Background Data Analysis (LAMBDA) at http://lambda.gsfc.nasa.gov, and Anthony Lewis and Sarah Bridle for making their CosmoMC software  available at http://cosmologist.info/cosmomc. Support for LAMBDA is provided by the NASA Office of Space Science. M.T. was supported by NASA Grants NAG5-11099 and NNG06GC55G, NSF Grants AST-0134999, and 0607597, the Kavli Foundation, and the David and Lucile Packard Foundation, and the Research Corporation. D.J.E. was supported by NSF Grant AST-0407200 and by the Alfred P. Sloan Foundation. Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.|
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|Deposited On:||01 Nov 2007|
|Last Modified:||26 Dec 2012 09:45|
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