Kinetic AGN feedback effects on cluster cool cores simulated using SPH

Autores
Barai, Paramita; Murante, Giuseppe; Borgani, Stefano; Gaspari, Massimo; Granato, Gian Luigi; Monaco, Pierluigi; Ragone Figueroa, Cinthia Judith
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We implement novel numerical models of AGN feedback in the SPH code gadget-3, where the energy from a supermassive black hole (BH) is coupled to the surrounding gas in the kinetic form. Gas particles lying inside a bi-conical volume around the BH are imparted a one-time velocity (10 000 km s-1) increment. We perform hydrodynamical simulations of isolated cluster (total mass 1014 h-1 M⊙), which is initially evolved to form a dense cool core, having central T ≤ 106 K. A BH resides at the cluster centre, and ejects energy. The feedback-driven fast wind undergoes shock with the slower moving gas, which causes the imparted kinetic energy to be thermalized. Bipolar bubble-like outflows form propagating radially outward to a distance of a few 100 kpc. The radial profiles of median gas properties are influenced by BH feedback in the inner regions (r < 20-50 kpc). BH kinetic feedback, with a large value of the feedback efficiency, depletes the inner cool gas and reduces the hot gas content, such that the initial cool core of the cluster is heated up within a time 1.9 Gyr, whereby the core median temperature rises to above 107 K, and the central entropy flattens. Our implementation of BH thermal feedback (using the same efficiency as kinetic), within the star formation model, cannot do this heating, where the cool core remains. The inclusion of cold gas accretion in the simulations produces naturally a duty cycle of the AGN with a periodicity of 100 Myr.
Fil: Barai, Paramita. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Murante, Giuseppe. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Borgani, Stefano. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Gaspari, Massimo. University of Princeton; Estados Unidos
Fil: Granato, Gian Luigi. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Monaco, Pierluigi. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Ragone Figueroa, Cinthia Judith. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Materia
BLACK HOLE PHYSICS
COSMOLOGY: THEORY
GALAXIES: CLUSTERS: GENERAL
GALAXIES: JETS
HYDRODYNAMICS
QUASARS: SUPERMASSIVE BLACK HOLES
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/183147
Acceder
id CONICETDig_8127ea630a2c42dae5697fd5d447fbbd
oai_identifier_str oai:ri.conicet.gov.ar:11336/183147
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Kinetic AGN feedback effects on cluster cool cores simulated using SPHBarai, ParamitaMurante, GiuseppeBorgani, StefanoGaspari, MassimoGranato, Gian LuigiMonaco, PierluigiRagone Figueroa, Cinthia JudithBLACK HOLE PHYSICSCOSMOLOGY: THEORYGALAXIES: CLUSTERS: GENERALGALAXIES: JETSHYDRODYNAMICSQUASARS: SUPERMASSIVE BLACK HOLEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We implement novel numerical models of AGN feedback in the SPH code gadget-3, where the energy from a supermassive black hole (BH) is coupled to the surrounding gas in the kinetic form. Gas particles lying inside a bi-conical volume around the BH are imparted a one-time velocity (10 000 km s-1) increment. We perform hydrodynamical simulations of isolated cluster (total mass 1014 h-1 M⊙), which is initially evolved to form a dense cool core, having central T ≤ 106 K. A BH resides at the cluster centre, and ejects energy. The feedback-driven fast wind undergoes shock with the slower moving gas, which causes the imparted kinetic energy to be thermalized. Bipolar bubble-like outflows form propagating radially outward to a distance of a few 100 kpc. The radial profiles of median gas properties are influenced by BH feedback in the inner regions (r < 20-50 kpc). BH kinetic feedback, with a large value of the feedback efficiency, depletes the inner cool gas and reduces the hot gas content, such that the initial cool core of the cluster is heated up within a time 1.9 Gyr, whereby the core median temperature rises to above 107 K, and the central entropy flattens. Our implementation of BH thermal feedback (using the same efficiency as kinetic), within the star formation model, cannot do this heating, where the cool core remains. The inclusion of cold gas accretion in the simulations produces naturally a duty cycle of the AGN with a periodicity of 100 Myr.Fil: Barai, Paramita. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; ItaliaFil: Murante, Giuseppe. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; ItaliaFil: Borgani, Stefano. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Consiglio Nazionale delle Ricerche; ItaliaFil: Gaspari, Massimo. University of Princeton; Estados UnidosFil: Granato, Gian Luigi. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; ItaliaFil: Monaco, Pierluigi. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia. Consiglio Nazionale delle Ricerche; ItaliaFil: Ragone Figueroa, Cinthia Judith. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaWiley Blackwell Publishing, Inc2016-09-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/183147Barai, Paramita; Murante, Giuseppe; Borgani, Stefano; Gaspari, Massimo; Granato, Gian Luigi; et al.; Kinetic AGN feedback effects on cluster cool cores simulated using SPH; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 461; 2; 11-9-2016; 1548-15670035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/461/2/1548/2608490info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stw1389info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1605.08051info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:20:38Zoai:ri.conicet.gov.ar:11336/183147instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 12:20:38.809CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Kinetic AGN feedback effects on cluster cool cores simulated using SPH
title Kinetic AGN feedback effects on cluster cool cores simulated using SPH
spellingShingle Kinetic AGN feedback effects on cluster cool cores simulated using SPH
Barai, Paramita
BLACK HOLE PHYSICS
COSMOLOGY: THEORY
GALAXIES: CLUSTERS: GENERAL
GALAXIES: JETS
HYDRODYNAMICS
QUASARS: SUPERMASSIVE BLACK HOLES
title_short Kinetic AGN feedback effects on cluster cool cores simulated using SPH
title_full Kinetic AGN feedback effects on cluster cool cores simulated using SPH
title_fullStr Kinetic AGN feedback effects on cluster cool cores simulated using SPH
title_full_unstemmed Kinetic AGN feedback effects on cluster cool cores simulated using SPH
title_sort Kinetic AGN feedback effects on cluster cool cores simulated using SPH
dc.creator.none.fl_str_mv Barai, Paramita
Murante, Giuseppe
Borgani, Stefano
Gaspari, Massimo
Granato, Gian Luigi
Monaco, Pierluigi
Ragone Figueroa, Cinthia Judith
author Barai, Paramita
author_facet Barai, Paramita
Murante, Giuseppe
Borgani, Stefano
Gaspari, Massimo
Granato, Gian Luigi
Monaco, Pierluigi
Ragone Figueroa, Cinthia Judith
author_role author
author2 Murante, Giuseppe
Borgani, Stefano
Gaspari, Massimo
Granato, Gian Luigi
Monaco, Pierluigi
Ragone Figueroa, Cinthia Judith
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv BLACK HOLE PHYSICS
COSMOLOGY: THEORY
GALAXIES: CLUSTERS: GENERAL
GALAXIES: JETS
HYDRODYNAMICS
QUASARS: SUPERMASSIVE BLACK HOLES
topic BLACK HOLE PHYSICS
COSMOLOGY: THEORY
GALAXIES: CLUSTERS: GENERAL
GALAXIES: JETS
HYDRODYNAMICS
QUASARS: SUPERMASSIVE BLACK HOLES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We implement novel numerical models of AGN feedback in the SPH code gadget-3, where the energy from a supermassive black hole (BH) is coupled to the surrounding gas in the kinetic form. Gas particles lying inside a bi-conical volume around the BH are imparted a one-time velocity (10 000 km s-1) increment. We perform hydrodynamical simulations of isolated cluster (total mass 1014 h-1 M⊙), which is initially evolved to form a dense cool core, having central T ≤ 106 K. A BH resides at the cluster centre, and ejects energy. The feedback-driven fast wind undergoes shock with the slower moving gas, which causes the imparted kinetic energy to be thermalized. Bipolar bubble-like outflows form propagating radially outward to a distance of a few 100 kpc. The radial profiles of median gas properties are influenced by BH feedback in the inner regions (r < 20-50 kpc). BH kinetic feedback, with a large value of the feedback efficiency, depletes the inner cool gas and reduces the hot gas content, such that the initial cool core of the cluster is heated up within a time 1.9 Gyr, whereby the core median temperature rises to above 107 K, and the central entropy flattens. Our implementation of BH thermal feedback (using the same efficiency as kinetic), within the star formation model, cannot do this heating, where the cool core remains. The inclusion of cold gas accretion in the simulations produces naturally a duty cycle of the AGN with a periodicity of 100 Myr.
Fil: Barai, Paramita. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Murante, Giuseppe. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Borgani, Stefano. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Gaspari, Massimo. University of Princeton; Estados Unidos
Fil: Granato, Gian Luigi. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Monaco, Pierluigi. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia. Consiglio Nazionale delle Ricerche; Italia
Fil: Ragone Figueroa, Cinthia Judith. Istituto Nazionale di Astrofisica; Italia. Consiglio Nazionale delle Ricerche; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
description We implement novel numerical models of AGN feedback in the SPH code gadget-3, where the energy from a supermassive black hole (BH) is coupled to the surrounding gas in the kinetic form. Gas particles lying inside a bi-conical volume around the BH are imparted a one-time velocity (10 000 km s-1) increment. We perform hydrodynamical simulations of isolated cluster (total mass 1014 h-1 M⊙), which is initially evolved to form a dense cool core, having central T ≤ 106 K. A BH resides at the cluster centre, and ejects energy. The feedback-driven fast wind undergoes shock with the slower moving gas, which causes the imparted kinetic energy to be thermalized. Bipolar bubble-like outflows form propagating radially outward to a distance of a few 100 kpc. The radial profiles of median gas properties are influenced by BH feedback in the inner regions (r < 20-50 kpc). BH kinetic feedback, with a large value of the feedback efficiency, depletes the inner cool gas and reduces the hot gas content, such that the initial cool core of the cluster is heated up within a time 1.9 Gyr, whereby the core median temperature rises to above 107 K, and the central entropy flattens. Our implementation of BH thermal feedback (using the same efficiency as kinetic), within the star formation model, cannot do this heating, where the cool core remains. The inclusion of cold gas accretion in the simulations produces naturally a duty cycle of the AGN with a periodicity of 100 Myr.
publishDate 2016
dc.date.none.fl_str_mv 2016-09-11
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/183147
Barai, Paramita; Murante, Giuseppe; Borgani, Stefano; Gaspari, Massimo; Granato, Gian Luigi; et al.; Kinetic AGN feedback effects on cluster cool cores simulated using SPH; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 461; 2; 11-9-2016; 1548-1567
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/183147
identifier_str_mv Barai, Paramita; Murante, Giuseppe; Borgani, Stefano; Gaspari, Massimo; Granato, Gian Luigi; et al.; Kinetic AGN feedback effects on cluster cool cores simulated using SPH; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 461; 2; 11-9-2016; 1548-1567
0035-8711
1365-2966
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/461/2/1548/2608490
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stw1389
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1605.08051
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1846782655733956608
score 12.982451

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