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Title: Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

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 NM1.2 ± 0.1 (NM0.68 ± 0.34) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad-band colours and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGNs luminosity function (LF). The LF exhibits a redshift trend of the form (1 + |$z$|)γ in density and luminosity, respectively, of γD = 3.0 ± 0.4 andmore » γP = 0.21 ± 0.15 in the RM-Y3 sample, and γD = 2.6 ± 0.7 and γP = 0.31 ± 0.15 in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGNs, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core (<0.1R500) X-ray radiative losses for clusters at |$z$| < 1.« less

Authors:
ORCiD logo [1];  [2];  [3];  [4];  [5];  [6]; ORCiD logo [7];  [8];  [9]; ORCiD logo [6];  [10]; ORCiD logo [11]; ORCiD logo [12];  [13]; ORCiD logo [14];  [2];  [15]; ORCiD logo [7];  [16];  [17] more »;  [9];  [18]; ORCiD logo [19];  [7]; ORCiD logo [20]; ORCiD logo [21];  [12];  [15];  [6];  [18];  [22];  [23];  [18];  [24]; ORCiD logo [25];  [26];  [15];  [27];  [28];  [12];  [29];  [15]; ORCiD logo [6];  [12]; ORCiD logo [30]; ORCiD logo [8];  [7];  [31];  [32];  [6];  [33];  [34];  [20];  [7];  [2]; ORCiD logo [35];  [36];  [2]; ORCiD logo [37];  [38];  [39];  [40] « less
  1. School of Physics, University of Melbourne, Parkville, VIC 3010, Australia, Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr 1, D-81679 Munich, Germany, Excellence Cluster Origins, Boltzmannstr 2, D-85748 Garching, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr, D-85748 Garching, Germany
  2. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr 1, D-81679 Munich, Germany
  3. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr 1, D-81679 Munich, Germany, Excellence Cluster Origins, Boltzmannstr 2, D-85748 Garching, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr, D-85748 Garching, Germany
  4. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr 1, D-81679 Munich, Germany, Max Planck Institute for Extraterrestrial Physics, Giessenbachstr, D-85748 Garching, Germany
  5. Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, P. O. Box 2450, Stanford, CA 94305, USA, SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
  6. Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA
  7. Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, Spain
  8. School of Physics, University of Melbourne, Parkville, VIC 3010, Australia
  9. Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
  10. Center for Astrophysics Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
  11. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain, Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil
  12. Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA, National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA
  13. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra, Barcelona, Spain
  14. Academia Sinica Institute of Astronomy and Astrophysics, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Section 4, Roosevelt Rd, Taipei 10617, Taiwan
  15. Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil, Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil
  16. Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India
  17. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr 1, D-81679 Munich, Germany, Excellence Cluster Origins, Boltzmannstr 2, D-85748 Garching, Germany
  18. Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, USA
  19. Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA, Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
  20. Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain, Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain
  21. Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, P. O. Box 2450, Stanford, CA 94305, USA, SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA
  22. Department of Physics, The Ohio State University, Columbus, OH 43210, USA
  23. Center for Astrophysics Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA
  24. Australian Astronomical Optics, Macquarie University, North Ryde, NSW 2113, Australia
  25. The Research School of Astronomy and Astrophysics, Australian National University, ACT 2601, Australia
  26. Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil, Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP 05314-970, Brazil
  27. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA
  28. Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
  29. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra, Barcelona, Spain, Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain
  30. Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA
  31. Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil, Instituto de Física, UFRGS, Caixa Postal 15051, Porto Alegre, RS 91501-970, Brazil
  32. INAF – Osservatorio Astronomico di Trieste, via Tiepolo 11, I-34143 Trieste, Italy, IFPU – Institute for Fundamental Physics of the Universe, Via Beirut 2, I-34014 Trieste, Italy, INAF – Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, I-34143 Trieste, Italy
  33. SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
  34. Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
  35. School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK
  36. Department of Physics, Lancaster University, Lancaster LA1 4YB, UK
  37. Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA
  38. National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA
  39. Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
  40. Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC); Argonne National Lab. (ANL), Argonne, IL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR)
Contributing Org.:
DES Collaboration
OSTI Identifier:
1616204
Alternate Identifier(s):
OSTI ID: 1615369; OSTI ID: 1638179; OSTI ID: 1659578; OSTI ID: 1756413
Report Number(s):
arXiv:1906.11388; DES-2019-0324; FERMILAB-PUB-19-204-AE
Journal ID: ISSN 0035-8711
Grant/Contract Number:  
AC02-05CH11231; AC02-07CH11359; AC02-76SF00515; PLR-1248097; AST-1138766; AST-1536171; GBMF 947; AYA2015-71825; ESP2015-66861; FPA2015-68048; SEV-2016-0588; SEV-2016-0597; MDM-2015-0509; FP7/2007-2013; 240672; 291329; 306478; 465376/2014-2; AC05-00OR22725; AC02-06CH11357
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 494 Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United Kingdom
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; galaxies: clusters: general; galaxies: active; galaxies: luminosity function, mass function; submillimeter: galaxies; cosmology: observations; galaxies; active; clusters; luminosity function; mass function; cosmology; observations; submillimeter

Citation Formats

Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chiu, I., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., McDonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1. United Kingdom: N. p., 2020. Web. doi:10.1093/mnras/staa832.
Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chiu, I., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., McDonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., & Zenteno, A. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1. United Kingdom. doi:https://doi.org/10.1093/mnras/staa832
Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chiu, I., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., McDonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A. Fri . "Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1". United Kingdom. doi:https://doi.org/10.1093/mnras/staa832.
@article{osti_1616204,
title = {Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1},
author = {Gupta, N. and Pannella, M. and Mohr, J. J. and Klein, M. and Rykoff, E. S. and Annis, J. and Avila, S. and Bianchini, F. and Brooks, D. and Buckley-Geer, E. and Bulbul, E. and Carnero Rosell, A. and Carrasco Kind, M. and Carretero, J. and Chiu, I. and Costanzi, M. and da Costa, L. N. and De Vicente, J. and Desai, S. and Dietrich, J. P. and Doel, P. and Everett, S. and Evrard, A. E. and García-Bellido, J. and Gaztanaga, E. and Gruen, D. and Gruendl, R. A. and Gschwend, J. and Gutierrez, G. and Hollowood, D. L. and Honscheid, K. and James, D. J. and Jeltema, T. and Kuehn, K. and Lidman, C. and Lima, M. and Maia, M. A. G. and Marshall, J. L. and McDonald, M. and Menanteau, F. and Miquel, R. and Ogando, R. L. C. and Palmese, A. and Paz-Chinchón, F. and Plazas, A. A. and Reichardt, C. L. and Sanchez, E. and Santiago, B. and Saro, A. and Scarpine, V. and Schindler, R. and Schubnell, M. and Serrano, S. and Sevilla-Noarbe, I. and Shao, X. and Smith, M. and Stott, J. P. and Strazzullo, V. and Suchyta, E. and Swanson, M. E. C. and Vikram, V. and Zenteno, A.},
abstractNote = {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 favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad-band colours and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGNs luminosity function (LF). The LF exhibits a redshift trend of the form (1 + |$z$|)γ in density and luminosity, respectively, of γD = 3.0 ± 0.4 and γP = 0.21 ± 0.15 in the RM-Y3 sample, and γD = 2.6 ± 0.7 and γP = 0.31 ± 0.15 in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGNs, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core (<0.1R500) X-ray radiative losses for clusters at |$z$| < 1.},
doi = {10.1093/mnras/staa832},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 494,
place = {United Kingdom},
year = {2020},
month = {4}
}

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DOI: https://doi.org/10.1093/mnras/staa832

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