Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 499, Issue 4, Pages 4768-4784Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa3044
Keywords
cosmological parameters; X-rays: galaxies: clusters
Categories
Funding
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- Brazilian Participation Group
- Carnegie Institution for Science
- Carnegie Mellon University
- Chilean Participation Group
- French Participation Group
- Harvard-Smithsonian Center for Astrophysics
- Instituto de Astrof'isica de Canarias
- Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam (AIP)
- MaxPlanck-Institut fur Astronomie (MPIA Heidelberg)
- Max-PlanckInstitut fur Astrophysik (MPA Garching)
- Max-Planck-Institut f ur Extraterrestrische Physik (MPE)
- National Astronomical Observatory of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observat 'ario Nacional/MCTI
- Ohio StateUniversity
- Pennsylvania State University
- ShanghaiAstronomical Observatory
- United Kingdom Participation Group
- Universidad Nacional Aut'onoma de M'exico
- University of Arizona
- University of Colorado Boulder
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
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This paper presents a cosmological analysis based on the properties of X-ray selected clusters of galaxies from the CODEX survey which have been spectroscopically followed up within the SPIDERS programme as part of the sixteenth data release (DR16) of SDSS-IV. The cosmological sub-sample contains a total of 691 clusters over an area of 5350 deg(2) with newly measured optical properties provided by a reanalysis of the CODEX source catalogue using redMaPPer and the DESI Legacy Imaging Surveys (DR8). Optical richness is used as a proxy for the cluster mass, and the combination of X-ray, optical, and spectroscopic information ensures that only confirmed virialized systems are considered. Clusters are binned in observed redshift, (z) over tilde is an element of [0.1, 0.6) and optical richness, (lambda) over tilde is an element of[25, 148) and the number of clusters in each bin is modelled as a function of cosmological and richness-mass scaling relation parameters. A high-purity sub-sample of 691 clusters is used in the analysis and best-fitting cosmological parameters are found to be Omega m(0) = 0.34(-0.05)(+0.09) and sigma(8) = 0.73(-0.03)(+0.03). The redshift evolution of the self-calibrated richness-mass relation is poorly constrained due to the systematic uncertainties associated with the X-ray component of the selection function (which assumes a fixed X-ray luminosity-mass relation with h = 0.7 and Omega m(0) = 0.30). Repeating the analysis with the assumption of no redshift evolution is found to improve the consistency between both cosmological and scaling relation parameters with respect to recent galaxy cluster analyses in the literature.
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