Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 444, Issue 1, Pages 476-502Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu1391
Keywords
galaxies: haloes; galaxies: statistics; cosmological parameters; large-scale structure of Universe
Categories
Funding
- Alfred P. Sloan Foundation
- National Science Foundation [PHYS-1066293]
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- NASA through Hubble Fellowship grant - Space Telescope Science Institute [51280]
- NASA [NAS 5-26555]
- World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan
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We perform the first fit to the anisotropic clustering of Sloan Digital Sky Survey III CMASS data release 10 galaxies on scales of similar to 0.8-32 h(-1) Mpc. A standard halo occupation distribution model evaluated near the best-fitting Planck Alpha cold dark matter (Lambda CDM) cosmology provides a good fit to the observed anisotropic clustering, and implies a normalization for the peculiar velocity field of M similar to 2 x 10(13)h(-1) M-circle dot haloes of f sigma(8)(z = 0.57) = 0.450 +/- 0.011. Since this constraint includes both quasi-linear and non-linear scales, it should severely constrain modified gravity models that enhance pairwise infall velocities on these scales. Though model dependent, our measurement represents a factor of 2.5 improvement in precision over the analysis of DR11 on large scales, f sigma(8)(z = 0.57) = 0.447 +/- 0.028, and is the tightest single constraint on the growth rate of cosmic structure to date. Our measurement is consistent with the Planck Lambda CDM prediction of 0.480 +/- 0.010 at the similar to 1.9 sigma level. Assuming a halo mass function evaluated at the best-fitting Planck cosmology, we also find that 10 per cent of CMASS galaxies are satellites in haloes of mass M similar to 6 x 10(13) h(-1) M-circle dot. While none of our tests and model generalizations indicate systematic errors due to an insufficiently detailed model of the galaxy-halo connection, the precision of these first results warrant further investigation into the modelling uncertainties and degeneracies with cosmological parameters.
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