Galaxy kinematics and mass calibration in massive SZE-selected galaxy clusters to z=1.3
R Capasso, A Saro, JJ Mohr, A Biviano, S Bocquet, V Strazzullo, S Grandis, DE Applegate, MB Bayliss, BA Benson, LE Bleem, M Brodwin, E Bulbul, JE Carlstrom, I Chiu, JP Dietrich, N Gupta, T de Haan, J Hlavacek-Larrondo, M Klein Show all
Monthly Notices of the Royal Astronomical Society | Oxford University Press (OUP) | Published : 2019
The galaxy phase-space distribution in galaxy clusters provides insights into the formation and evolution of cluster galaxies, and it can also be used to measure cluster mass profiles. We present a dynamical study based on ~3000 passive, non-emission-line cluster galaxies drawn from 110 galaxy clusters. The galaxy clusters were selected using the Sunyaev-Zel'dovich effect (SZE) in the 2500 deg 2 South Pole Telescope (SPT)-SZ survey and cover the redshift range 0.2 < z < 1.3. We model the clusters using the Jeans equation, while adopting NFW mass profiles and a broad range of velocity dispersion anisotropy profiles. The data prefer velocity dispersion anisotropy profiles that are approximatel..View full abstract
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Awarded by National Science Foundation
Awarded by NSF Physics Frontier Center
Awarded by Gordon and Betty Moore Foundation
Awarded by Australian Research Council
Awarded by U.S. Department of Energy
Awarded by Fermi Research Alliance, LLC
Awarded by ERC-StG 'ClustersXCosmo'
We thank Cristobal Sifon for providing useful feedback. We acknowledge the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe', the Transregio program TR33 'The Dark Universe', and the Ludwig-Maximilians University (LMU). 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. The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects funding scheme (DP150103208). DR is supported by a NASA Postdoctoral Program Senior Fellowship at NASA's Ames Research Center, administered by the Universities Space Research Association under contract with NASA. Work at Argonne National Laboratory was supported under U.S. Department of Energy contract DE-AC02-06CH11357. AB acknowledges the hospitality of the LMU, and partial financial support from PRIN-INAF 2014 'Glittering kaleidoscopes in the sky: the multifaceted nature and role of Galaxy Clusters' (PI: Mario Nonino). BB has been supported by the Fermi Research Alliance, LLC under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. AS is supported by the ERC-StG 'ClustersXCosmo', grant agreement no. 716762.