Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 407, Issue 1, Pages 533-543Publisher
WILEY-BLACKWELL
DOI: 10.1111/j.1365-2966.2010.16930.x
Keywords
galaxies: clusters: general; cosmological parameters
Categories
Funding
- National Natural Science Foundation (NNSF) of China [10773016, 10821061, 1083303]
- National Key Basic Research Science Foundation of China [2007CB815403]
- Liaoning Educational Foundation of China [2009A646, XN200902, 054-55440105020]
- Alfred P. Sloan Foundation
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- Cambridge University
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max Planck Institute for Astronomy (MPIA)
- Max Planck Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
- National Science Foundation
- U.S. Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
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The mass function of galaxy clusters is a powerful tool to constrain cosmological parameters, e.g. the mass fluctuation on the scale of 8 h-1 Mpc, Sigma(8), and the abundance of total matter, (m). We first determine the scaling relations between cluster mass and cluster richness, summed r-band luminosity and the global galaxy number within a cluster radius. These relations are then used to two complete volume-limited rich cluster samples which we obtained from the Sloan Digital Sky Survey (SDSS). We estimate the masses of these clusters and determine the cluster mass function. Fitting the data with a theoretical expression, we get the cosmological parameter constraints in the form of Sigma(8)((m)/0.3)alpha = beta and find out the parameters of alpha = 0.40-0.50 and beta = 0.8-0.9, so that Sigma(8) = 0.8-0.9 if (m) = 0.3. Our Sigma(8) value is slightly higher than recent estimates from the mass function of X-ray clusters and the Wilkinson Microwave Anisotropy Probe (WMAP) data, but consistent with the weak lensing statistics.
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