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Cosmological Constraints from Galaxy Clusters in the 2500 Square-degree SPT-SZ Survey

de Haan, T. and Crites, A. T. and Padin, S. and Williamson, R. (2016) Cosmological Constraints from Galaxy Clusters in the 2500 Square-degree SPT-SZ Survey. Astrophysical Journal, 832 (1). Art. No. 95. ISSN 0004-637X. doi:10.3847/0004-637X/832/1/95.

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We present cosmological parameter constraints obtained from galaxy clusters identified by their Sunyaev–Zel'dovich effect signature in the 2500 square-degree South Pole Telescope Sunyaev Zel'dovich (SPT-SZ) survey. We consider the 377 cluster candidates identified at z > 0.25 with a detection significance greater than five, corresponding to the 95% purity threshold for the survey. We compute constraints on cosmological models using the measured cluster abundance as a function of mass and redshift. We include additional constraints from multi-wavelength observations, including Chandra X-ray data for 82 clusters and a weak lensing-based prior on the normalization of the mass-observable scaling relations. Assuming a spatially flat ΛCDM cosmology, we combine the cluster data with a prior on H 0 and find σ_8 = 0.784 ± 0.039 and Ω_m = 0.289 ± 0.042, with the parameter combination σ_8(Ω_m/0.27)^(0.3) = 0.797 ± 0.031. These results are in good agreement with constraints from the cosmic microwave background (CMB) from SPT, WMAP, and Planck, as well as with constraints from other cluster data sets. We also consider several extensions to ΛCDM, including models in which the equation of state of dark energy w, the species-summed neutrino mass, and/or the effective number of relativistic species (N_(eff)) are free parameters. When combined with constraints from the Planck CMB, H_0, baryon acoustic oscillation, and SNe, adding the SPT cluster data improves the w constraint by 14%, to w = -1.023 ± 0.042.

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Additional Information:© 2016 The American Astronomical Society. Received 2016 March 21; revised 2016 August 15; accepted 2016 September 7; published 2016 November 18. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. This work used resources of McGill University's High Performance Computing centre, a part of Compute Canada. This work was supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. TdH is supported by a Miller Research Fellowship, as well as receiving support from a Natural Science and Engineering Research Council of Canada Postgraduate Scholarship-Doctoral award. BB is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. Argonne National Laboratory's work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. DA and TS acknowledge support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under projects 50 OR 1210 and 50 OR 1407. RJF gratefully acknowledges support from the Alfred P. Sloan Foundation. CR acknowledges support from the University of Melbourne and from the Australian Research Council's Discovery Projects scheme (DP150103208). JHL is supported by NSERC through the discovery grant and Canada Research Chair programs, as well as FRQNT. The Munich group acknowledges the support of the DFG Cluster of Excellence "Origin and Structure of the universe" and the Transregio program TR33 "The Dark universe." The Dark Cosmology Centre is funded by the Danish National Research Foundation. Optical and infrared followup of SPT Clusters at the Harvard-Smithsonian Center for Astrophysics was supported by NSF grant ANT-1009649.
Funding AgencyGrant Number
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF 947
Department of Energy (DOE)DE-AC02-76SF00515
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canada Research Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Miller Research FellowshipUNSPECIFIED
Department of Energy (DOE)DE-AC02-07CH11359
Department of Energy (DOE)DE-AC02-06CH11357
Deutsche Zentrum für Luft- und Raumfahrt (DLR)50 OR 1210
Deutsche Zentrum für Luft- und Raumfahrt (DLR)50 OR 1407
Alfred P. Sloan FoundationUNSPECIFIED
University of MelbourneUNSPECIFIED
Australian Research CouncilDP150103208
Fonds Québécois de la Recherche sur la Nature et les Technologies (FQRNT)UNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)TR33 Dark Universe
Bundesministerium für Wirtschaft und Energie (BMWi)UNSPECIFIED
Danish National Research FoundationUNSPECIFIED
Subject Keywords:cosmology: observations – galaxies: clusters: general
Issue or Number:1
Record Number:CaltechAUTHORS:20161122-121544091
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Official Citation:T. de Haan et al 2016 ApJ 832 95
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72247
Deposited By: Tony Diaz
Deposited On:22 Nov 2016 22:22
Last Modified:11 Nov 2021 04:58

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