Phys. Rev. D
74,
123507
(2006)
[34 pages]
Cosmological constraints from the SDSS luminous red galaxies
Max Tegmark et al.
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Max Tegmark1, Daniel J. Eisenstein2, Michael A. Strauss3, David H. Weinberg4, Michael R. Blanton5, Joshua A. Frieman6,7, Masataka Fukugita8, James E. Gunn3, Andrew J. S. Hamilton9, Gillian R. Knapp3, Robert C. Nichol10, Jeremiah P. Ostriker3, Nikhil Padmanabhan11, Will J. Percival10, David J. Schlegel12, Donald P. Schneider13, Roman Scoccimarro5, Uroš Seljak11,14, Hee-Jong Seo2, Molly Swanson1, Alexander S. Szalay15, Michael S. Vogeley16, Jaiyul Yoo4, Idit Zehavi17, Kevork Abazajian18, Scott F. Anderson19, James Annis7, Neta A. Bahcall3, Bruce Bassett20,21, Andreas Berlind5, Jon Brinkmann22, Tamás Budavari15, Francisco Castander23, Andrew Connolly24, Istvan Csabai15, Mamoru Doi25, Douglas P. Finkbeiner3,26, Bruce Gillespie22, Karl Glazebrook15, Gregory S. Hennessy27, David W. Hogg5, Željko Ivezić3,19, Bhuvnesh Jain28, David Johnston29,30, Stephen Kent7, Donald Q. Lamb6,31, Brian C. Lee12,32, Huan Lin7, Jon Loveday33, Robert H. Lupton3, Jeffrey A. Munn27, Kaike Pan22, Changbom Park34, John Peoples7, Jeffrey R. Pier27, Adrian Pope15, Michael Richmond35, Constance Rockosi6, Ryan Scranton24, Ravi K. Sheth28, Albert Stebbins7, Christopher Stoughton7, István Szapudi36, Douglas L. Tucker7, Daniel E. Vanden Berk24, Brian Yanny7, and Donald G. York6,31
1Department of Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
2Department of Astronomy, University of Arizona, Tucson, Arizona 85721, USA
3Princeton University Observatory, Princeton, New Jersey 08544, USA
4Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA
5Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, New York 10003, USA
6Center for Cosmological Physics and Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
7Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, Illinois 60510, USA
8Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba, 277-8582, Japan
9JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
10Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, P01 2EG, United Kingdom
11Department of Physics, Princeton University, Princeton, New Jersey 08544, USA
12Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
13Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
14International Center for Theoretical Physics, Strada Costiera 11, 34014 Trieste, Italy
15Department of Physics and Astronomy, The Johns Hopkins University, 3701 San Martin Drive, Baltimore, Maryland 21218, USA
16Department of Physics, Drexel University, Philadelphia, Pennsylvania 19104, USA
17Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, Ohio 44106-7215, USA
18Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
19Department of Astronomy, University of Washington, Box 351580, Seattle, Washington 98195, USA
20South African Astronomical Observatory, Cape Town, South Africa;
21Applied Mathematics Department, University of Cape Town, Cape Town, South Africa
22Apache Point Observatory, 2001 Apache Point Road, Sunspot, New Mexico 88349-0059, USA
23Institut d’Estudis Espacials de Catalunya/CSIC, Campus UAB, 08034 Barcelona, Spain
24University of Pittsburgh, Department of Physics and Astronomy, 3941 O’Hara Street, Pittsburgh, Pennsylvania 15260, USA
25Institute of Astronomy, University of Tokyo, Osawa 2-21-1, Mitaka, Tokyo, 181-0015, Japan
26Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS46, Cambridge, Massachusetts 02138, USA
27U.S. Naval Observatory, Flagstaff Station, 10391 W. Naval Observatory Road, Flagstaff, Arizona 86001-8521, USA
28Department of Physics, University of Pennsylvania, Philadelphia, Pennsylvania 19104, USA
29Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena California, 91109, USA;
30California Institute of Technology, 1200 East California Boulevard, Pasadena, California 91125, USA
31Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA
32Gatan Inc., Pleasanton, California 94588, USA
33Sussex Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QJ, UK
34Department of Astronomy, Seoul National University, 151-742, Korea
35Physics Department, Rochester Institute of Technology, 1 Lomb Memorial Dr, Rochester, New York 14623, USA
36Institute for Astronomy, University of Hawaii, 2680, Woodlawn Drive, Honolulu, Hawaii 96822, USA
Received 22 August 2006; published 11 December 2006
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 ΛCDM 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 Ωm and the baryon fraction in good agreement with WMAP. Within the context of flat ΛCDM 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 Ωm=0.24±0.02 (1σ), ∑mν≲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 ΛCDM framework, our power spectrum measurement improves the evidence for spatial flatness, sharpening the curvature constraint Ωtot=1.05±0.05 from WMAP alone to Ωtot=1.003±0.010. Assuming Ωtot=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.
© 2006 The American Physical Society
URL:
http://link.aps.org/doi/10.1103/PhysRevD.74.123507
DOI:
10.1103/PhysRevD.74.123507
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