The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, MBH, and the galaxy bulge or stellar mass, M*. The cosmic evolution of this relation, though, is still a matter...

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Detalles Bibliográficos
Autor: Mountrichas, George
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:dnet:digitalcsic_::23c67db519d0b336e435af3ecdea0eda
Acceso en línea:http://hdl.handle.net/10261/336066
Access Level:acceso abierto
Palabra clave:Galaxies: active
Galaxies: evolution
Quasars: supermassive black holes
Galaxies: star formation
X-rays: galaxies
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spelling The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshiftMountrichas, GeorgeGalaxies: activeGalaxies: evolutionQuasars: supermassive black holesGalaxies: star formationX-rays: galaxiesIt is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, MBH, and the galaxy bulge or stellar mass, M*. The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the MBH − M* relation, using 687 X-ray luminous (median log [LX,2−10 keV(erg s−1)] = 44.3), broad-line active galactic nuclei (AGN), at 0.2 <  z <  4.0 (median z ≈ 1.4) that lie in the XMM-XXL field. Their MBH and M* range from 7.5 <  log [MBH (M⊙)] <  9.5 and 10 <  log [M*(M⊙)] <  12, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that MBH and M* are correlated (r = 0.47 ± 0.21, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the MBH and M* does not evolve with redshift, at least up to z = 2 and has a value of log(MBH/M*)= − 2.44. The majority of the AGN (75%) are in a SMBH mass growth-dominant phase. In these systems, the MBH − M* correlation is weaker and their M* tends to be lower (for the same MBH) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.The author acknowledges support by the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. This project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement no 101004168, the XMM2ATHENA project. This research has made use of TOPCAT version 4.8 (Taylor 2005).Peer reviewedEDP SciencesMinisterio de Ciencia, Innovación y Universidades (España)Agencia Estatal de Investigación (España)European CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/336066reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI//MDM-2017-0765info:eu-repo/grantAgreement/EC/H2020/101004168https://doi.org/10.1051/0004-6361/202345924Síinfo:eu-repo/semantics/openAccessoai:dnet:digitalcsic_::23c67db519d0b336e435af3ecdea0eda2026-05-22T06:33:51Z
dc.title.none.fl_str_mv The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
title The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
spellingShingle The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
Mountrichas, George
Galaxies: active
Galaxies: evolution
Quasars: supermassive black holes
Galaxies: star formation
X-rays: galaxies
title_short The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
title_full The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
title_fullStr The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
title_full_unstemmed The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
title_sort The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift
dc.creator.none.fl_str_mv Mountrichas, George
author Mountrichas, George
author_facet Mountrichas, George
author_role author
dc.contributor.none.fl_str_mv Ministerio de Ciencia, Innovación y Universidades (España)
Agencia Estatal de Investigación (España)
European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Galaxies: active
Galaxies: evolution
Quasars: supermassive black holes
Galaxies: star formation
X-rays: galaxies
topic Galaxies: active
Galaxies: evolution
Quasars: supermassive black holes
Galaxies: star formation
X-rays: galaxies
description It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, MBH, and the galaxy bulge or stellar mass, M*. The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the MBH − M* relation, using 687 X-ray luminous (median log [LX,2−10 keV(erg s−1)] = 44.3), broad-line active galactic nuclei (AGN), at 0.2 <  z <  4.0 (median z ≈ 1.4) that lie in the XMM-XXL field. Their MBH and M* range from 7.5 <  log [MBH (M⊙)] <  9.5 and 10 <  log [M*(M⊙)] <  12, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that MBH and M* are correlated (r = 0.47 ± 0.21, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the MBH and M* does not evolve with redshift, at least up to z = 2 and has a value of log(MBH/M*)= − 2.44. The majority of the AGN (75%) are in a SMBH mass growth-dominant phase. In these systems, the MBH − M* correlation is weaker and their M* tends to be lower (for the same MBH) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/336066
url http://hdl.handle.net/10261/336066
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/AEI//MDM-2017-0765
info:eu-repo/grantAgreement/EC/H2020/101004168
https://doi.org/10.1051/0004-6361/202345924
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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