The mass and galaxy distribution around SZ-selected clusters

Creators: Shin, T.; Jain, B.; Adhikari, S.; Baxter, E. J.; Chang, C.; Pandey, S.; Salcedo, A.; Weinberg, D. H.; Amsellem, A.; Battaglia, N.; Belyakov, M.; Dacunha, T.; Goldstein, S.; Kravtsov, A. V.; Varga, T. N.; Abbott, T. M. C.; Aguena, M.; Alarcon, A.; Allam, S.; Amon, A.; Andrade-Oliveira, F.; Annis, J.; Bacon, D.; Bechtol, K.; Becker, M. R.; Bernstein, G. M.; Bertin, E.; Bocquet, S.; Bond, J. R.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Campos, A.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Chen, R.; Choi, A.; Costanzi, M.; da Costa, L. N.; DeRose, J.; Desai, S.; De Vicente, J.; Devlin, M. J.; Diehl, H. T.; Dietrich, J. P.; Dodelson, S.; Doel, P.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Elvin-Poole, J.; Everett, S.; Ferraro, S.; Ferrero, I.; Ferté, A.; Flaugher, B.; Frieman, J.; Gallardo, P. A.; Gatti, M.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Harrison, I.; Hartley, W. G.; Hill, J. C.; Hilton, M.; Hinton, S. R.; Hollowood, D. L.; Hughes, J. P.; James, D. J.; Jarvis, M.; Jeltema, T.; Koopman, B. J.; Krause, E.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Lokken, M.; MacCrann, N.; Madhavacheril, M. S.; Maia, M. A. G.; McCullough, J.; McMahon, J.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr, J. J.; Moodley, K.; Morgan, R.; Myles, J.; Nati, F.; Navarro-Alsina, A.; Niemack, M. D.; Ogando, R. L. C.; Page, L. A.; Palmese, A.; Partridge, B.; Paz-Chinchón, F.; Pereira, M. E. S.; Pieres, A.; Plazas Malagón, A. A.; Prat, J.; Raveri, M.; Rodriguez-Monroy, M.; Rollins, R. P.; Romer, A. K.; Rykoff, E. S.; Salatino, M.; Sánchez, C.; Sanchez, E.; Santiago, B.; Scarpine, V.; Schillaci, A.; Secco, L. F.; Serrano, S.; Sevilla-Noarbe, I.; Sheldon, E.; Sherwin, B. D.; Sifón, C.; Smith, M.; Soares-Santos, M.; Staggs, S. T.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; To, C.; Troxel, M. A.; Tutusaus, I.; Vavagiakis, E. M.; Weller, J.; Wollack, E. J.; Yanny, B.; Yin, B.; Zhang, Y.

Abstract

We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev–Zel'dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 data set. With signal-to-noise ratio of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2–20 h⁻¹ Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. (2) The full mass profile is also consistent with the simulations. (3) The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift, and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology, and astrophysics are discussed.

Additional Information

© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2021 August 26. Received 2021 August 25; in original form 2021 May 13. Published: 07 September 2021. We thank Neal Dalal and Ravi Sheth for stimulating discussions. We are grateful to Phil Mansfield, Chun-Hao To for comments on the draft. The CosmoSim data base used in this paper is a service by the Leibniz-Institute for Astrophysics Potsdam (AIP). The MultiDark database was developed in cooperation with the Spanish MultiDark Consolider Project CSD2009-00064. We gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gauss-centre.eu) and the Partnership for Advanced Supercomputing in Europe (PRACE, www.prace-ri.eu) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, www.lrz.de). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Centre for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant no. 465376/2014-2). This manuscript has been authored by 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. The ACT project is supported by the U.S. National Science Foundation through awards AST-1440226, AST-0965625, and AST-0408698, as well as awards PHY-1214379 and PHY-0855887. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación Científica y Tecnológica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium and on the hippo cluster at the University of KwaZulu-Natal. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund – Research Excellence; and the University of Toronto. The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Work at Argonne National Laboratory was supported under U.S. Department of Energy contract DEAC02-06CH11357. JPH acknowledges funding for SZ cluster studies from NSF AAG number AST-1615657. Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science and Industry Canada and by the Province of Ontario through the Ministry of Colleges and Universities. KM acknowledges support from the National Research Foundation of South Africa. Data Availability: The data underlying this article will be shared on reasonable request to the corresponding author.

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