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T.S. and M.M. acknowledge support from the Kavli Research Investment Fund at MIT, and from NASA through Chandra grant GO5-16143.F.R. acknowledges financial support provided by NASA through SAO Award Number SV2-82023 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060.This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.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.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 Center 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, FundacAo Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e InovacAo, 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 Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians-Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the OzDES Membership Consortium, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.

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The Evolution of AGN Activity in Brightest Cluster Galaxies

Publicado en:ASTRONOMICAL JOURNAL. 163 (4): 146- - 2022-04-01 163(4), DOI: 10.3847/1538-3881/ac5030

Autores: Somboonpanyakul, T; McDonald, M; Calzadilla, M; Ruppin, F; Amon, A; Burke, DL; To, C; Noble, A; Aguena, M; Andrade-Oliveira, F; Rosell, AC; da Costa, LN; Gschwend, J; Lima, M; Maia, MAG; Ogando, RLC; Pieres, A; Allam, S; Buckley-Geer, E; Flaugher, B; Gutierrez, G; Palmese, A; Scarpine, V; Tucker, DL; Bacon, D; Bayliss, MB; Kim, KJ; Bertin, E; Bhargava, S; Romer, AK; Wilkinson, RD; Brooks, D; Doel, P; Khullar, G; Reil, K; Canning, R; Kind, MC; Gruendl, RA; Menanteau, F; Paz-Chinchón, F; Swanson, MEC; Carretero, J; Miquel, R; Costanzi, M; Saro, A; Singh, P; Strazzullo, V; Pereira, MES; Evrard, AE; Gerdes, DW; Schubnell, M; Soares-Santos, M; Tarle, G; De Vicente, J; Sanchez, E; Sevilla-Noarbe, I; Eisenhardt, P; Everett, S; Hollowood, DL; Jeltema, T; Ferrero, I; Floyd, B; García-Bellido, J; Gaztanaga, E; Serrano, S; Gonzalez, A; Gruen, D; Hoyle, B; Klein, M; Mohr, JJ; Gupta, N; Hinton, SR; Honscheid, K; Martini, P; James, DJ; Kuehn, K; Marshall, JL; Melchior, P; Malagón, AAP; Morgan, R; Smith, M; Suchyta, E

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We present the results of an analysis of Wide-field Infrared Survey Explorer (WISE) observations of the full 2500 deg(2) South Pole Telescope (SPT)-Sunyaev-Zel'dovich cluster sample. We describe a process for identifying active galactic nuclei (AGN) in brightest cluster galaxies (BCGs) based on WISE mid-IR color and redshift. Applying this technique to the BCGs of the SPT-SZ sample, we calculate the AGN-hosting BCG fraction, which is defined as the fraction of BCGs hosting bright central AGNs over all possible BCGs. Assuming an evolving single-burst stellar population model, we find statistically significant evidence (>99.9%) for a mid-IR excess at high redshift compared to low redshift, suggesting that the fraction of AGN-hosting BCGs increases with redshift over the range of 0 < z < 1.3. The best-fit redshift trend of the AGN-hosting BCG fraction has the form (1 + z)(4.1 +/- 1.0). These results are consistent with previous studies in galaxy clusters as well as as in field galaxies. One way to explain this result is that member galaxies at high redshift tend to have more cold gas. While BCGs in nearby galaxy clusters grow mostly by dry mergers with cluster members, leading to no increase in AGN activity, BCGs at high redshift could primarily merge with gas-rich satellites, providing fuel for feeding AGNs. If this observed increase in AGN activity is linked to gas-rich mergers rather than ICM cooling, we would expect to see an increase in scatter in the P (cav) versus L (cool) relation at z > 1. Last, this work confirms that the runaway cooling phase, as predicted by the classical cooling-flow model, in the Phoenix cluster is extremely rare and most BCGs have low (relative to Eddington) black hole accretion rates.

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