Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 401, Issue 4, Pages 2477-2489Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2009.15824.x
Keywords
methods: statistical; galaxies: clusters: general; cosmology: observations; large-scale structure of Universe
Categories
Funding
- PPARC/STFC
- ETF [7146]
- Alfred P. Sloan Foundation
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- 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 Grou
- 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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We use the direct Fourier method to calculate the redshift-space power spectrum of the maxBCG cluster catalogue - currently by far the largest existing galaxy cluster sample. The total number of clusters used in our analysis is 12 616. After accounting for the radial smearing effect caused by photometric redshift errors and also introducing a simple treatment for the non-linear effects, we show that currently favoured low matter density 'concordance' Lambda cold dark matter cosmology provides a very good fit to the estimated power. Thanks to the large volume (similar to 0.4 h(-3) Gpc(3)), high clustering amplitude [linear effective bias parameter b(eff) similar to 3 x (0.85/sigma(8))] and sufficiently high sampling density (similar to 3 x 10(-5) h(3) Mpc(-3)), the recovered power spectrum has a high enough signal-to-noise ratio to allow us to find weak evidence [similar to 2 sigma confidence level (CL)] for the baryonic acoustic oscillations (BAO). In case the clusters are additionally weighted by their richness, the resulting power spectrum has slightly higher large-scale amplitude and smaller damping on small scales. As a result, the CL for the BAO detection is somewhat increased: similar to 2.5 sigma. The ability to detect BAO with a relatively small number of clusters is encouraging in the light of several proposed large cluster surveys.
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