On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium
- Autores
- Planelles, Susana; Borgani, Stefano; Fabjan, Dunja; Killedar, Madhura; Murante, Giuseppe; Granato, Gian Luigi; Ragone Figueroa, Cinthia Judith; Dolag, Klaus
- Año de publicación
- 2014
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present an analysis of the properties of the intracluster medium (ICM) in an extended set of cosmological hydrodynamical simulations of galaxy clusters and groups performed with the . treepm+. sph . gadget-3 code. Besides a set of non-radiative simulations, we carried out two sets of simulations including radiative cooling, star formation, metal enrichment and feedback from supernovae (SNe), one of which also accounts for the effect of feedback from active galactic nuclei (AGN) resulting from gas accretion on to supermassive black holes. These simulations are analysed with the aim of studying the relative role played by SN and AGN feedback on the general properties of the diffuse hot baryons in galaxy clusters and groups: scaling relations, temperature, entropy and pressure radial profiles, and ICM chemical enrichment. We find that simulations including AGN feedback produce scaling relations between X-ray observable quantities that are in good agreement with observations at all mass scales. Observed pressure profiles are also shown to be quite well reproduced in our radiative simulations, especially when AGN feedback is included. However, our simulations are not able to account for the observed diversity between cool-core and non-cool-core clusters, as revealed by X-ray observations: unlike for observations, we find that temperature and entropy profiles of relaxed and unrelaxed clusters are quite similar and resemble more the observed behaviour of non-cool-core clusters. As for the pattern of metal enrichment, we find that an enhanced level of iron abundance is produced by AGN feedback with respect to the case of purely SN feedback. As a result, while simulations including AGN produce values of iron abundance in groups in agreement with observations, they over-enrich the ICM in massive clusters. The efficiency of AGN feedback in displacing enriched gas from haloes into the intergalactic medium at high redshift also creates a widespread enrichment in the outskirts of clusters and produces profiles of iron abundance whose slope is in better agreement with observations. By analysing the pattern of the relative abundances of silicon and iron and the fraction of metals in the stellar phase, our results clearly show that different sources of energy feedback leave different imprints in the enrichment pattern of the hot ICM and stars. Our results confirm that including AGN feedback goes in the right direction of reconciling simulation predictions and observations for several observational ICM properties. Still a number of important discrepancies highlight that the model still needs to be improved to produce the correct interplay between cooling and feedback in central cluster regions. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Fil: Planelles, Susana. Università degli Studi di Trieste; Italia
Fil: Borgani, Stefano. Istituto Nazionale di Astrofisica; Italia
Fil: Fabjan, Dunja. Istituto Nazionale di Astrofisica; Italia. Slovenian Centre Of Excellence For Space Sciences And Technologies; Eslovenia. Univerza V Ljubljani; Eslovenia
Fil: Killedar, Madhura. Osservatorio Astronomico Di Trieste; Italia
Fil: Murante, Giuseppe. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronomico Di Trieste; Italia
Fil: Granato, Gian Luigi. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronomico Di Trieste; Italia
Fil: Ragone Figueroa, Cinthia Judith. Osservatorio Astronomico Di Trieste; 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
Fil: Dolag, Klaus. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania - Materia
-
COSMOLOGY: MISCELLANEOUS
GALAXIES: CLUSTERS: GENERAL
METHODS: NUMERICAL
X-RAYS: GALAXIES - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/183610
Ver los metadatos del registro completo
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On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster mediumPlanelles, SusanaBorgani, StefanoFabjan, DunjaKilledar, MadhuraMurante, GiuseppeGranato, Gian LuigiRagone Figueroa, Cinthia JudithDolag, KlausCOSMOLOGY: MISCELLANEOUSGALAXIES: CLUSTERS: GENERALMETHODS: NUMERICALX-RAYS: GALAXIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present an analysis of the properties of the intracluster medium (ICM) in an extended set of cosmological hydrodynamical simulations of galaxy clusters and groups performed with the . treepm+. sph . gadget-3 code. Besides a set of non-radiative simulations, we carried out two sets of simulations including radiative cooling, star formation, metal enrichment and feedback from supernovae (SNe), one of which also accounts for the effect of feedback from active galactic nuclei (AGN) resulting from gas accretion on to supermassive black holes. These simulations are analysed with the aim of studying the relative role played by SN and AGN feedback on the general properties of the diffuse hot baryons in galaxy clusters and groups: scaling relations, temperature, entropy and pressure radial profiles, and ICM chemical enrichment. We find that simulations including AGN feedback produce scaling relations between X-ray observable quantities that are in good agreement with observations at all mass scales. Observed pressure profiles are also shown to be quite well reproduced in our radiative simulations, especially when AGN feedback is included. However, our simulations are not able to account for the observed diversity between cool-core and non-cool-core clusters, as revealed by X-ray observations: unlike for observations, we find that temperature and entropy profiles of relaxed and unrelaxed clusters are quite similar and resemble more the observed behaviour of non-cool-core clusters. As for the pattern of metal enrichment, we find that an enhanced level of iron abundance is produced by AGN feedback with respect to the case of purely SN feedback. As a result, while simulations including AGN produce values of iron abundance in groups in agreement with observations, they over-enrich the ICM in massive clusters. The efficiency of AGN feedback in displacing enriched gas from haloes into the intergalactic medium at high redshift also creates a widespread enrichment in the outskirts of clusters and produces profiles of iron abundance whose slope is in better agreement with observations. By analysing the pattern of the relative abundances of silicon and iron and the fraction of metals in the stellar phase, our results clearly show that different sources of energy feedback leave different imprints in the enrichment pattern of the hot ICM and stars. Our results confirm that including AGN feedback goes in the right direction of reconciling simulation predictions and observations for several observational ICM properties. Still a number of important discrepancies highlight that the model still needs to be improved to produce the correct interplay between cooling and feedback in central cluster regions. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.Fil: Planelles, Susana. Università degli Studi di Trieste; ItaliaFil: Borgani, Stefano. Istituto Nazionale di Astrofisica; ItaliaFil: Fabjan, Dunja. Istituto Nazionale di Astrofisica; Italia. Slovenian Centre Of Excellence For Space Sciences And Technologies; Eslovenia. Univerza V Ljubljani; EsloveniaFil: Killedar, Madhura. Osservatorio Astronomico Di Trieste; ItaliaFil: Murante, Giuseppe. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronomico Di Trieste; ItaliaFil: Granato, Gian Luigi. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronomico Di Trieste; ItaliaFil: Ragone Figueroa, Cinthia Judith. Osservatorio Astronomico Di Trieste; 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; ArgentinaFil: Dolag, Klaus. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaWiley Blackwell Publishing, Inc2014-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/183610Planelles, Susana; Borgani, Stefano; Fabjan, Dunja; Killedar, Madhura; Murante, Giuseppe; et al.; On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 438; 1; 1-2014; 195-2160035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2014MNRAS.438..195Pinfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stt2141info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:52:27Zoai:ri.conicet.gov.ar:11336/183610instacron: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:34982025-09-29 09:52:27.42CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
title |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
spellingShingle |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium Planelles, Susana COSMOLOGY: MISCELLANEOUS GALAXIES: CLUSTERS: GENERAL METHODS: NUMERICAL X-RAYS: GALAXIES |
title_short |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
title_full |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
title_fullStr |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
title_full_unstemmed |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
title_sort |
On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium |
dc.creator.none.fl_str_mv |
Planelles, Susana Borgani, Stefano Fabjan, Dunja Killedar, Madhura Murante, Giuseppe Granato, Gian Luigi Ragone Figueroa, Cinthia Judith Dolag, Klaus |
author |
Planelles, Susana |
author_facet |
Planelles, Susana Borgani, Stefano Fabjan, Dunja Killedar, Madhura Murante, Giuseppe Granato, Gian Luigi Ragone Figueroa, Cinthia Judith Dolag, Klaus |
author_role |
author |
author2 |
Borgani, Stefano Fabjan, Dunja Killedar, Madhura Murante, Giuseppe Granato, Gian Luigi Ragone Figueroa, Cinthia Judith Dolag, Klaus |
author2_role |
author author author author author author author |
dc.subject.none.fl_str_mv |
COSMOLOGY: MISCELLANEOUS GALAXIES: CLUSTERS: GENERAL METHODS: NUMERICAL X-RAYS: GALAXIES |
topic |
COSMOLOGY: MISCELLANEOUS GALAXIES: CLUSTERS: GENERAL METHODS: NUMERICAL X-RAYS: GALAXIES |
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 present an analysis of the properties of the intracluster medium (ICM) in an extended set of cosmological hydrodynamical simulations of galaxy clusters and groups performed with the . treepm+. sph . gadget-3 code. Besides a set of non-radiative simulations, we carried out two sets of simulations including radiative cooling, star formation, metal enrichment and feedback from supernovae (SNe), one of which also accounts for the effect of feedback from active galactic nuclei (AGN) resulting from gas accretion on to supermassive black holes. These simulations are analysed with the aim of studying the relative role played by SN and AGN feedback on the general properties of the diffuse hot baryons in galaxy clusters and groups: scaling relations, temperature, entropy and pressure radial profiles, and ICM chemical enrichment. We find that simulations including AGN feedback produce scaling relations between X-ray observable quantities that are in good agreement with observations at all mass scales. Observed pressure profiles are also shown to be quite well reproduced in our radiative simulations, especially when AGN feedback is included. However, our simulations are not able to account for the observed diversity between cool-core and non-cool-core clusters, as revealed by X-ray observations: unlike for observations, we find that temperature and entropy profiles of relaxed and unrelaxed clusters are quite similar and resemble more the observed behaviour of non-cool-core clusters. As for the pattern of metal enrichment, we find that an enhanced level of iron abundance is produced by AGN feedback with respect to the case of purely SN feedback. As a result, while simulations including AGN produce values of iron abundance in groups in agreement with observations, they over-enrich the ICM in massive clusters. The efficiency of AGN feedback in displacing enriched gas from haloes into the intergalactic medium at high redshift also creates a widespread enrichment in the outskirts of clusters and produces profiles of iron abundance whose slope is in better agreement with observations. By analysing the pattern of the relative abundances of silicon and iron and the fraction of metals in the stellar phase, our results clearly show that different sources of energy feedback leave different imprints in the enrichment pattern of the hot ICM and stars. Our results confirm that including AGN feedback goes in the right direction of reconciling simulation predictions and observations for several observational ICM properties. Still a number of important discrepancies highlight that the model still needs to be improved to produce the correct interplay between cooling and feedback in central cluster regions. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Fil: Planelles, Susana. Università degli Studi di Trieste; Italia Fil: Borgani, Stefano. Istituto Nazionale di Astrofisica; Italia Fil: Fabjan, Dunja. Istituto Nazionale di Astrofisica; Italia. Slovenian Centre Of Excellence For Space Sciences And Technologies; Eslovenia. Univerza V Ljubljani; Eslovenia Fil: Killedar, Madhura. Osservatorio Astronomico Di Trieste; Italia Fil: Murante, Giuseppe. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronomico Di Trieste; Italia Fil: Granato, Gian Luigi. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronomico Di Trieste; Italia Fil: Ragone Figueroa, Cinthia Judith. Osservatorio Astronomico Di Trieste; 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 Fil: Dolag, Klaus. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania |
description |
We present an analysis of the properties of the intracluster medium (ICM) in an extended set of cosmological hydrodynamical simulations of galaxy clusters and groups performed with the . treepm+. sph . gadget-3 code. Besides a set of non-radiative simulations, we carried out two sets of simulations including radiative cooling, star formation, metal enrichment and feedback from supernovae (SNe), one of which also accounts for the effect of feedback from active galactic nuclei (AGN) resulting from gas accretion on to supermassive black holes. These simulations are analysed with the aim of studying the relative role played by SN and AGN feedback on the general properties of the diffuse hot baryons in galaxy clusters and groups: scaling relations, temperature, entropy and pressure radial profiles, and ICM chemical enrichment. We find that simulations including AGN feedback produce scaling relations between X-ray observable quantities that are in good agreement with observations at all mass scales. Observed pressure profiles are also shown to be quite well reproduced in our radiative simulations, especially when AGN feedback is included. However, our simulations are not able to account for the observed diversity between cool-core and non-cool-core clusters, as revealed by X-ray observations: unlike for observations, we find that temperature and entropy profiles of relaxed and unrelaxed clusters are quite similar and resemble more the observed behaviour of non-cool-core clusters. As for the pattern of metal enrichment, we find that an enhanced level of iron abundance is produced by AGN feedback with respect to the case of purely SN feedback. As a result, while simulations including AGN produce values of iron abundance in groups in agreement with observations, they over-enrich the ICM in massive clusters. The efficiency of AGN feedback in displacing enriched gas from haloes into the intergalactic medium at high redshift also creates a widespread enrichment in the outskirts of clusters and produces profiles of iron abundance whose slope is in better agreement with observations. By analysing the pattern of the relative abundances of silicon and iron and the fraction of metals in the stellar phase, our results clearly show that different sources of energy feedback leave different imprints in the enrichment pattern of the hot ICM and stars. Our results confirm that including AGN feedback goes in the right direction of reconciling simulation predictions and observations for several observational ICM properties. Still a number of important discrepancies highlight that the model still needs to be improved to produce the correct interplay between cooling and feedback in central cluster regions. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. |
publishDate |
2014 |
dc.date.none.fl_str_mv |
2014-01 |
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/11336/183610 Planelles, Susana; Borgani, Stefano; Fabjan, Dunja; Killedar, Madhura; Murante, Giuseppe; et al.; On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 438; 1; 1-2014; 195-216 0035-8711 1365-2966 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/183610 |
identifier_str_mv |
Planelles, Susana; Borgani, Stefano; Fabjan, Dunja; Killedar, Madhura; Murante, Giuseppe; et al.; On the role of AGN feedback on the thermal and chemodynamical properties of the hot intracluster medium; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 438; 1; 1-2014; 195-216 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/http://adsabs.harvard.edu/abs/2014MNRAS.438..195P info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stt2141 |
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 |
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1844613609127149568 |
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13.070432 |