期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 424, 期 3, 页码 2339-2344出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2012.21404.x
关键词
surveys; Cosmology: observations; dark energy - large-scale structure of Universe
资金
- European Research Council
- National Science Foundation [AST-0901965]
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy
- 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
- STFC [ST/H002774/1, ST/I001204/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/H002774/1, ST/I001204/1] Funding Source: researchfish
- ICREA Funding Source: Custom
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0901965] Funding Source: National Science Foundation
We explore the benefits of using a passively evolving population of galaxies to measure the evolution of the rate of structure growth between z = 0.25 and 0.65 by combining data from the Sloan Digital Sky Survey (SDSS) I/II and SDSS-III surveys. The large-scale linear bias of a population of dynamically passive galaxies, which we select from both surveys, is easily modelled. Knowing the bias evolution breaks degeneracies inherent to other methodologies, and decreases the uncertainty in measurements of the rate of structure growth and the normalization of the galaxy power spectrum by up to a factor of 2. If we translate our measurements into a constraint on s8(z = 0) assuming a concordance cosmological model and general relativity (GR), we find that using a bias model improves our uncertainty by a factor of nearly 1.5. Our results are consistent with a flat ? cold dark matter model and with GR.
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