The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?

We recently discovered that the active galactic nucleus (AGN) of Mrk 1018 has changed optical type again after 30 yr as a type 1 AGN. Here we combine Chandra, NuStar, Swift, Hubble Space Telescope and ground-based observations to explore the cause of this change. The 2-10 keV flux declines by a fact...

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Autores: Husemann, B., Urrutia, T., Tremblay, G. R., Krumpe, M., Dexter, J., Busch, G., Combes, F., Croom, S. M., Davis, T. A., Eckart, Andreas, McElroy, R. E., Pérez-Torres, Miguel A., Powell, M., Scharwächter, J.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2016
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/377229
Acceso en línea:http://hdl.handle.net/10261/377229
Access Level:acceso abierto
Palabra clave:Accretion, accretion disks
Galaxies: nuclei
Galaxies: Seyfert
Galaxies: individual: Mrk 1018
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spelling The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?Husemann, B.Urrutia, T.Tremblay, G. R.Krumpe, M.Dexter, J.Busch, G.Combes, F.Croom, S. M.Davis, T. A.Eckart, AndreasMcElroy, R. E.Pérez-Torres, Miguel A.Powell, M.Scharwächter, J.Accretion, accretion disksGalaxies: nucleiGalaxies: SeyfertGalaxies: individual: Mrk 1018We recently discovered that the active galactic nucleus (AGN) of Mrk 1018 has changed optical type again after 30 yr as a type 1 AGN. Here we combine Chandra, NuStar, Swift, Hubble Space Telescope and ground-based observations to explore the cause of this change. The 2-10 keV flux declines by a factor of ∼8 between 2010 and 2016. We show with our X-ray observation that this is not caused by varying neutral hydrogen absorption along the line-of-sight up to the Compton-thick level. The optical-UV spectral energy distributions are well fit with a standard geometrically thin optically thick accretion disc model that seems to obey the expected L ∼ T relation. It confirms that a decline in accretion disc luminosity is the primary origin for the type change. We detect a new narrow-line absorber in Lyα blue-shifted by ∼700 km s with respect to the systemic velocity of the galaxy. This new Lyα absorber could be evidence for the onset of an outflow or a companion black hole with associated gas that could be related to the accretion rate change. However, the low column density of the absorber means that it is not the direct cause for Mrk 1018's changing-look nature. © ESO, 2016.We thank the anonymous referee for very constructive comments and suggestions that significantly helped to improve this Letter. GRT acknowledges support from the NASA through the Einstein Postdoctoral Fellowship Award Number PF-150128, 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. MK acknowledges support by DFG grant KR 3338/3-1. MAPT acknowledges support from the Spanish MINECO through grants AYA2012-38491-C02-02 and AYA2015-63939-C2-1-P. TAD acknowledges support from a Science and Technology Facilities Council Ernest Rutherford Fellowship. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.Peer reviewedEDP SciencesNASAGerman Research FoundationMinisterio de Economía y Competitividad (España)Science and Technology Facilities Council (UK)Australian Research CouncilConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520162025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/377229reponame: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/MINECO//AYA2012-38491-C02-02info:eu-repo/grantAgreement/MINECO//AYA2015-63939-C2-1-Phttp://dx.doi.org/10.1051/0004-6361/201629245Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3772292026-05-22T06:33:51Z
dc.title.none.fl_str_mv The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
title The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
spellingShingle The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
Husemann, B.
Accretion, accretion disks
Galaxies: nuclei
Galaxies: Seyfert
Galaxies: individual: Mrk 1018
title_short The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
title_full The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
title_fullStr The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
title_full_unstemmed The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
title_sort The Close AGN Reference Survey (CARS): What is causing Mrk 1018's return to the shadows after 30 years?
dc.creator.none.fl_str_mv Husemann, B.
Urrutia, T.
Tremblay, G. R.
Krumpe, M.
Dexter, J.
Busch, G.
Combes, F.
Croom, S. M.
Davis, T. A.
Eckart, Andreas
McElroy, R. E.
Pérez-Torres, Miguel A.
Powell, M.
Scharwächter, J.
author Husemann, B.
author_facet Husemann, B.
Urrutia, T.
Tremblay, G. R.
Krumpe, M.
Dexter, J.
Busch, G.
Combes, F.
Croom, S. M.
Davis, T. A.
Eckart, Andreas
McElroy, R. E.
Pérez-Torres, Miguel A.
Powell, M.
Scharwächter, J.
author_role author
author2 Urrutia, T.
Tremblay, G. R.
Krumpe, M.
Dexter, J.
Busch, G.
Combes, F.
Croom, S. M.
Davis, T. A.
Eckart, Andreas
McElroy, R. E.
Pérez-Torres, Miguel A.
Powell, M.
Scharwächter, J.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv NASA
German Research Foundation
Ministerio de Economía y Competitividad (España)
Science and Technology Facilities Council (UK)
Australian Research Council
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Accretion, accretion disks
Galaxies: nuclei
Galaxies: Seyfert
Galaxies: individual: Mrk 1018
topic Accretion, accretion disks
Galaxies: nuclei
Galaxies: Seyfert
Galaxies: individual: Mrk 1018
description We recently discovered that the active galactic nucleus (AGN) of Mrk 1018 has changed optical type again after 30 yr as a type 1 AGN. Here we combine Chandra, NuStar, Swift, Hubble Space Telescope and ground-based observations to explore the cause of this change. The 2-10 keV flux declines by a factor of ∼8 between 2010 and 2016. We show with our X-ray observation that this is not caused by varying neutral hydrogen absorption along the line-of-sight up to the Compton-thick level. The optical-UV spectral energy distributions are well fit with a standard geometrically thin optically thick accretion disc model that seems to obey the expected L ∼ T relation. It confirms that a decline in accretion disc luminosity is the primary origin for the type change. We detect a new narrow-line absorber in Lyα blue-shifted by ∼700 km s with respect to the systemic velocity of the galaxy. This new Lyα absorber could be evidence for the onset of an outflow or a companion black hole with associated gas that could be related to the accretion rate change. However, the low column density of the absorber means that it is not the direct cause for Mrk 1018's changing-look nature. © ESO, 2016.
publishDate 2016
dc.date.none.fl_str_mv 2016
2025
2025
2025
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/10261/377229
url http://hdl.handle.net/10261/377229
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/MINECO//AYA2012-38491-C02-02
info:eu-repo/grantAgreement/MINECO//AYA2015-63939-C2-1-P
http://dx.doi.org/10.1051/0004-6361/201629245
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
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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score 15,81155

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