Galaxy kinematics and mass calibration in massive SZE-selected galaxy clusters to z = 1.3

Journal Article · Mon Oct 01 00:00:00 EDT 2018 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/sty2645· OSTI ID:1479839

Capasso, R.  ^[1]; Saro, A. ^[2]; Mohr, J. J. ^[3]; Biviano, A. ^[4]; Bocquet, S. ^[5]; Strazzullo, V. ^[6]; Grandis, S. ^[1]; Applegate, D. E. ^[7]; Bayliss, M. B. ^[8]; Benson, B. A. ^[9]; Bleem, L. E. ^[10]; Brodwin, M. ^[11]; Bulbul, E. ^[8]; Carlstrom, J. E. ^[12]; Chiu, I. ^[13]; Dietrich, J. P. ^[1]; Gupta, N. ^[1]; de Haan, T. ^[14]; Hlavacek-Larrondo, J. ^[15]; Klein, M. ^[16] ; von der Linden, A. ^[17]; McDonald, M. ^[8]; Rapetti, D. ^[18]; Reichardt, C. L. ^[19]; Sharon, K. ^[20]; Stalder, B. ^[21]; Stanford, S. A. ^[22]; Stark, A. A. ^[21]; Stern, C. ^[1]; Zenteno, A. ^[23]

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1. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany, Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany
2. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany, Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany, INAF – Osservatorio Astronomico di Trieste via G.B. Tiepolo 11, I-34143 Trieste, Italy
3. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany, Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr., D-85748 Garching, Germany
4. INAF – Osservatorio Astronomico di Trieste via G.B. Tiepolo 11, I-34143 Trieste, Italy
5. Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA
6. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany
7. Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
8. Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
9. Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA, Fermi National Accelerator Laboratory, Batavia, IL 60510-0500, USA
10. Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA, Department of Physics, University of Chicago, Chicago, IL 60637, USA
11. Department of Physics and Astronomy, University of Missouri, 5110 Rockhill Road, Kansas City, MO 64110, USA
12. Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA, Department of Physics, University of Chicago, Chicago, IL 60637, USA, Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
13. Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 10617, Taiwan
14. Department of Physics, University of California, Berkeley, CA 94720, USA, Department of Physics, McGill University, Montreal, Quebec H3A 2T8, Canada
15. Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305-4085, USA, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA, Department of Physics, Université de Montréal, Montrea, Quebec H3T 1J4, Canada
16. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr., D-85748 Garching, Germany
17. Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305-4085, USA, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA, Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794, USA, Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
18. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany, Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany, Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA, NASA Ames Research Center, Moffett Field, CA 94035, USA
19. School of Physics, University of Melbourne, Parkville, VIC 3010, Australia
20. Department of Astronomy, University of Michigan, 1085 S. University Ave, Ann Arbor, MI 48109, USA
21. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
22. Department of Physics, University of California, Davis, CA 95616, USA, Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, Livermore, CA 94551, USA
23. Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile

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 $$\sim$$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$^2$ 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 approximately isotropic near the center and increasingly radial toward the cluster virial radius, and this is true for all redshifts and masses we study. The pseudo-phase-space density profile of the passive galaxies is consistent with expectations for dark matter particles and subhalos from cosmological $$N$$-body simulations. The dynamical mass constraints are in good agreement with external mass estimates of the SPT cluster sample from either weak lensing, velocity dispersions, or X-ray $$Y_X$$ measurements. However, the dynamical masses are lower (at the 2.2$$\sigma$$ level) when compared to the mass calibration favored when fitting the SPT cluster data to a $$\Lambda$$CDM model with external cosmological priors, including CMB anisotropy data from Planck. The discrepancy grows with redshift, where in the highest redshift bin the ratio of dynamical to SPT+Planck masses is $$\eta=0.63^{+0.13}_{-0.08}\pm0.06$$ (statistical and systematic), corresponding to a $$2.6\sigma$$ discrepancy.

• Research Organization: Argonne National Laboratory (ANL), Argonne, IL (United States); Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP)
• Contributing Organization: SPT
• Grant/Contract Number: AC02-06CH11357; AC02-07CH11359
• OSTI ID: 1479839
• Alternate ID(s): OSTI ID: 1413675
• Report Number(s): arXiv:1711.09903; FERMILAB-PUB-17-571-AE
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Vol. 482 Journal Issue: 1; ISSN 0035-8711
• Publisher: Royal Astronomical Society
• Country of Publication: United Kingdom
• Language: English

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79 ASTRONOMY AND ASTROPHYSICS