Journal article

Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z similar to 1

N Gupta, M Pannella, JJ Mohr, M Klein, ES Rykoff, J Annis, S Avila, F Bianchini, D Brooks, E Buckley-Geer, E Bulbul, A Carnero Rosell, M Carrasco Kind, J Carretero, I Chiu, M Costanzi, LN da Costa, J De Vicente, S Desai, JP Dietrich Show all

Monthly Notices of the Royal Astronomical Society | Oxford University Press (OUP) | Published : 2020

Abstract

We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843 MHz radio active galactic nuclei (AGNs) population in galaxy clusters from two large catalogues created using the Dark Energy Survey (DES): ∼11 800 optically selected RM-Y3 and ∼1000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGNs are highly concentrated around cluster centres to z ∼ 1. We measure the halo occupation number for cluster radio AGNs above a threshold luminosity, finding that the number of radio AGNs per cluster increases with cluster halo mass as N ∝ M1.2 ± 0.1 (N ∝ M0.68 ± 0.34) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favou..

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University of Melbourne Researchers

Grants

Awarded by Australian Research Council's Discovery Projects scheme


Awarded by Verbundforschung 'D-MeerKAT' award


Awarded by ERC-StG 'ClustersXCosmo' grant


Awarded by FARE-MIUR grant 'ClustersXEuclid'


Awarded by National Science Foundation


Awarded by NSF Physics Frontier Center grant


Awarded by Gordon and Betty Moore Foundation grant


Awarded by Office of Science of the U.S. Department of Energy


Awarded by MINECO


Awarded by E2RCgrant


Awarded by Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant)


Awarded by U.S. Department of Energy, Office of Science, Office of High Energy Physics


Funding Acknowledgements

We thank Jeremy Sanders for helpful discussions. The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). The Munich group acknowledges the support of the International Max Planck Research School on Astrophysics of the Ludwig-MaximiliansUniversitat, the Max-Planck-Gesellschaft Faculty Fellowship program at the Max Planck Institute for Extraterrestrial Physics, the DFG Cluster of Excellence 'Origin and Structure of the Universe', the Verbundforschung 'D-MeerKAT' award 05A2017 and the Ludwig-Maximilians-Universitat. AS is supported by the ERC-StG 'ClustersXCosmo' grant agreement 71676, and by the FARE-MIUR grant 'ClustersXEuclid' R165SBKTMA.SPT 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 research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.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 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 MINECO under grants AYA201571825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, 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 E2RCgrant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 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. TheUnited StatesGovernment retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. 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 United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paidup, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.