Phys. Rev. D
69,
103501
(2004)
[26 pages]
Cosmological parameters from SDSS and WMAP
Max Tegmark et al.
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Max Tegmark1,2, Michael A. Strauss3, Michael R. Blanton4, Kevork Abazajian5, Scott Dodelson6,7, Havard Sandvik1, Xiaomin Wang1, David H. Weinberg8, Idit Zehavi9, Neta A. Bahcall3, Fiona Hoyle10, David Schlegel3, Roman Scoccimarro4, Michael S. Vogeley10, Andreas Berlind7, Tamás Budavari11, Andrew Connolly12, Daniel J. Eisenstein9, Douglas Finkbeiner3, Joshua A. Frieman7,6, James E. Gunn3, Lam Hui6, Bhuvnesh Jain1, David Johnston7,6, Stephen Kent6, Huan Lin6, Reiko Nakajima1, Robert C. Nichol13, Jeremiah P. Ostriker3, Adrian Pope11, Ryan Scranton12, Uroš Seljak3, Ravi K. Sheth12, Albert Stebbins6, Alexander S. Szalay11, István Szapudi14, Yongzhong Xu5, James Annis6, J. Brinkmann15, Scott Burles2, Francisco J. Castander16, Istvan Csabai11, Jon Loveday17, Mamoru Doi18, Masataka Fukugita18, Bruce Gillespie15, Greg Hennessy19, David W. Hogg4, Željko Ivezić3, Gillian R. Knapp3, Don Q. Lamb7, Brian C. Lee6, Robert H. Lupton3, Timothy A. McKay20, Peter Kunszt11, Jeffrey A. Munn19, Liam O’Connell17, John Peoples6, Jeffrey R. Pier19, Michael Richmond21, Constance Rockosi7, Donald P. Schneider22, Christopher Stoughton6, Douglas L. Tucker6, Daniel E. Vanden Berk12, Brian Yanny6, and Donald G. York7,23
1Department of Physics, University of Pennsylvania, Philadelphia, Pennsylvania 19104, USA
2Department of Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
3Princeton University Observatory, Princeton, New Jersey 08544, USA
4Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, New York 10003, USA
5Theoretical Division, MS B285, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
6Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, Illinois 60510, USA
7Center for Cosmological Physics and Department of Astronomy & Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
8Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA
9Department of Astronomy, University of Arizona, Tucson, Arizona 85721, USA
10Department of Physics, Drexel University, Philadelphia, Pennsylvania 19104, USA
11Department of Physics and Astronomy, The Johns Hopkins University, 3701 San Martin Drive, Baltimore, Maryland 21218, USA
12University of Pittsburgh, Department of Physics and Astronomy, 3941 O’Hara Street, Pittsburgh, Pennsylvania 15260, USA
13Department of Physics, 5000 Forbes Avenue, Carnegie Mellon University, Pittsburgh, Pennsylvania 15213, USA
14Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA
15Apache Point Observatory, 2001 Apache Point Rd, Sunspot, New Mexico 88349-0059, USA
16Institut d’Estudis Espacials de Catalunya/CSIC, Gran Capita 2-4, 08034 Barcelona, Spain
17Sussex Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QJ, United Kingdom
18Institute of Astronomy, University of Tokyo, Kashiwa 277-8582, Japan
19U.S. Naval Observatory, Flagstaff Station, Flagstaff, Arizona 86002-1149, USA
20Department of Physics, University of Michigan, Ann Arbor, Michigan 48109-1120, USA
21Physics Department, Rochester Institute of Technology, 1 Lomb Memorial Drive, Rochester, New York 14623, USA
22Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
23Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA
Received 28 October 2003; published 5 May 2004
We measure cosmological parameters using the three-dimensional power spectrum P(k) from over 200 000 galaxies in the Sloan Digital Sky Survey (SDSS) in combination with Wilkinson Microwave Anisotropy Probe (WMAP) and other data. Our results are consistent with a “vanilla” flat adiabatic cold dark matter model with a cosmological constant without tilt (ns=1), running tilt, tensor modes, or massive neutrinos. Adding SDSS information more than halves the WMAP-only error bars on some parameters, tightening 1σ constraints on the Hubble parameter from h≈0.74-0.07+0.18 to h≈0.70-0.03+0.04, on the matter density from Ωm≈0.25±0.10 to Ωm≈0.30±0.04 (1σ) and on neutrino masses from <11 to <0.6eV (95%). SDSS helps even more when dropping prior assumptions about curvature, neutrinos, tensor modes and the equation of state. Our results are in substantial agreement with the joint analysis of WMAP and the Two Degree Field Galaxy Redshift Survey, which is an impressive consistency check with independent redshift survey data and analysis techniques. In this paper, we place particular emphasis on clarifying the physical origin of the constraints, i.e., what we do and do not know when using different data sets and prior assumptions. For instance, dropping the assumption that space is perfectly flat, the WMAP-only constraint on the measured age of the Universe tightens from t0≈16.3-1.8+2.3Gyr to t0≈14.1-0.9+1.0Gyr by adding SDSS and SN Ia data. Including tensors, running tilt, neutrino mass and equation of state in the list of free parameters, many constraints are still quite weak, but future cosmological measurements from SDSS and other sources should allow these to be substantially tightened.
© 2004 The American Physical Society
URL:
http://link.aps.org/doi/10.1103/PhysRevD.69.103501
DOI:
10.1103/PhysRevD.69.103501
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