Pressure of the hot gas in simulations of galaxy clusters

Autores
Planelles, S.; Fabjan, D.; Borgani, S.; Murante, G.; Rasia, E.; Biffi, V.; Truong, N.; Ragone Figueroa, Cinthia Judith; Granato, G. L.; Dolag, K.; Pierpaoli, E.; Beck, A. M.; Steinborn, Lisa K.; Gaspari, M.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We analyse the radial pressure profiles, the intracluster medium (ICM) clumping factor and the Sunyaev-Zel'dovich (SZ) scaling relations of a sample of simulated galaxy clusters and groups identified in a set of hydrodynamical simulations based on an updated version of the TREEPM-SPH GADGET-3 code. Three different sets of simulations are performed: the first assumes non-radiative physics, the others include, among other processes, active galactic nucleus (AGN) and/or stellar feedback. Our results are analysed as a function of redshift, ICM physics, cluster mass and cluster cool-coreness or dynamical state. In general, the mean pressure profiles obtained for our sample of groups and clusters show a good agreement with X-ray and SZ observations. Simulated cool-core (CC) and non-cool-core (NCC) clusters also show a good match with real data. We obtain in all cases a small (if any) redshift evolution of the pressure profiles of massive clusters, at least back to z = 1. We find that the clumpiness of gas density and pressure increases with the distance from the cluster centre and with the dynamical activity. The inclusion of AGN feedback in our simulations generates values for the gas clumping ( √ Cρ ~ 1.2 at R200) in good agreement with recent observational estimates. The simulated YSZ-Mscaling relations are in good accordance with several observed samples, especially for massive clusters. As for the scatter of these relations, we obtain a clear dependence on the cluster dynamical state, whereas this distinction is not so evident when looking at the subsamples of CC and NCC clusters.
Fil: Planelles, S.. Universidad de Valencia; España. Università degli Studi di Trieste; Italia
Fil: Fabjan, D.. Istituto Nazionale di Astrofisica; Italia. University of Ljubljana. Faculty of Mathematics and Physics; Argentina
Fil: Borgani, S.. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. University of Ljubljana. Faculty of Mathematics and Physics; Argentina
Fil: Murante, G.. Istituto Nazionale di Astrofisica; Italia
Fil: Rasia, E.. Istituto Nazionale di Astrofisica; Italia. University of Michigan; Estados Unidos
Fil: Biffi, V.. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Truong, N.. Università degli Studi di Roma Tor Vergata; Italia
Fil: Ragone Figueroa, Cinthia Judith. 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. Istituto Nazionale di Astrofisica; Italia
Fil: Granato, G. L.. Istituto Nazionale di Astrofisica; Italia
Fil: Dolag, K.. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania. University Observatory Munich; Alemania
Fil: Pierpaoli, E.. University of Southern California; Estados Unidos
Fil: Beck, A. M.. University Observatory Munich; Alemania
Fil: Steinborn, Lisa K.. University Observatory Munich; Alemania
Fil: Gaspari, M.. University of Princeton; Estados Unidos
Materia
GALAXIES: CLUSTERS: GENERAL -X-RAYS: GALAXIES: CLUSTERS
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
METHODS: NUMERICAL
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:11336/64102
Acceder
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Pressure of the hot gas in simulations of galaxy clustersPlanelles, S.Fabjan, D.Borgani, S.Murante, G.Rasia, E.Biffi, V.Truong, N.Ragone Figueroa, Cinthia JudithGranato, G. L.Dolag, K.Pierpaoli, E.Beck, A. M.Steinborn, Lisa K.Gaspari, M.GALAXIES: CLUSTERS: GENERAL -X-RAYS: GALAXIES: CLUSTERSGALAXIES: CLUSTERS: INTRACLUSTER MEDIUMMETHODS: NUMERICALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We analyse the radial pressure profiles, the intracluster medium (ICM) clumping factor and the Sunyaev-Zel'dovich (SZ) scaling relations of a sample of simulated galaxy clusters and groups identified in a set of hydrodynamical simulations based on an updated version of the TREEPM-SPH GADGET-3 code. Three different sets of simulations are performed: the first assumes non-radiative physics, the others include, among other processes, active galactic nucleus (AGN) and/or stellar feedback. Our results are analysed as a function of redshift, ICM physics, cluster mass and cluster cool-coreness or dynamical state. In general, the mean pressure profiles obtained for our sample of groups and clusters show a good agreement with X-ray and SZ observations. Simulated cool-core (CC) and non-cool-core (NCC) clusters also show a good match with real data. We obtain in all cases a small (if any) redshift evolution of the pressure profiles of massive clusters, at least back to z = 1. We find that the clumpiness of gas density and pressure increases with the distance from the cluster centre and with the dynamical activity. The inclusion of AGN feedback in our simulations generates values for the gas clumping ( √ Cρ ~ 1.2 at R200) in good agreement with recent observational estimates. The simulated YSZ-Mscaling relations are in good accordance with several observed samples, especially for massive clusters. As for the scatter of these relations, we obtain a clear dependence on the cluster dynamical state, whereas this distinction is not so evident when looking at the subsamples of CC and NCC clusters.Fil: Planelles, S.. Universidad de Valencia; España. Università degli Studi di Trieste; ItaliaFil: Fabjan, D.. Istituto Nazionale di Astrofisica; Italia. University of Ljubljana. Faculty of Mathematics and Physics; ArgentinaFil: Borgani, S.. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. University of Ljubljana. Faculty of Mathematics and Physics; ArgentinaFil: Murante, G.. Istituto Nazionale di Astrofisica; ItaliaFil: Rasia, E.. Istituto Nazionale di Astrofisica; Italia. University of Michigan; Estados UnidosFil: Biffi, V.. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Truong, N.. Università degli Studi di Roma Tor Vergata; ItaliaFil: Ragone Figueroa, Cinthia Judith. 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. Istituto Nazionale di Astrofisica; ItaliaFil: Granato, G. L.. Istituto Nazionale di Astrofisica; ItaliaFil: Dolag, K.. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania. University Observatory Munich; AlemaniaFil: Pierpaoli, E.. University of Southern California; Estados UnidosFil: Beck, A. M.. University Observatory Munich; AlemaniaFil: Steinborn, Lisa K.. University Observatory Munich; AlemaniaFil: Gaspari, M.. University of Princeton; Estados UnidosOxford University Press2017-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/64102Planelles, S.; Fabjan, D.; Borgani, S.; Murante, G.; Rasia, E.; et al.; Pressure of the hot gas in simulations of galaxy clusters; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 467; 4; 6-2017; 3827-38470035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/467/4/3827/2973007info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx318info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1612.07260v1info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:20:18Zoai:ri.conicet.gov.ar:11336/64102instacron: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:34982025-10-15 14:20:18.749CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Pressure of the hot gas in simulations of galaxy clusters
title Pressure of the hot gas in simulations of galaxy clusters
spellingShingle Pressure of the hot gas in simulations of galaxy clusters
Planelles, S.
GALAXIES: CLUSTERS: GENERAL -X-RAYS: GALAXIES: CLUSTERS
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
METHODS: NUMERICAL
title_short Pressure of the hot gas in simulations of galaxy clusters
title_full Pressure of the hot gas in simulations of galaxy clusters
title_fullStr Pressure of the hot gas in simulations of galaxy clusters
title_full_unstemmed Pressure of the hot gas in simulations of galaxy clusters
title_sort Pressure of the hot gas in simulations of galaxy clusters
dc.creator.none.fl_str_mv Planelles, S.
Fabjan, D.
Borgani, S.
Murante, G.
Rasia, E.
Biffi, V.
Truong, N.
Ragone Figueroa, Cinthia Judith
Granato, G. L.
Dolag, K.
Pierpaoli, E.
Beck, A. M.
Steinborn, Lisa K.
Gaspari, M.
author Planelles, S.
author_facet Planelles, S.
Fabjan, D.
Borgani, S.
Murante, G.
Rasia, E.
Biffi, V.
Truong, N.
Ragone Figueroa, Cinthia Judith
Granato, G. L.
Dolag, K.
Pierpaoli, E.
Beck, A. M.
Steinborn, Lisa K.
Gaspari, M.
author_role author
author2 Fabjan, D.
Borgani, S.
Murante, G.
Rasia, E.
Biffi, V.
Truong, N.
Ragone Figueroa, Cinthia Judith
Granato, G. L.
Dolag, K.
Pierpaoli, E.
Beck, A. M.
Steinborn, Lisa K.
Gaspari, M.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: CLUSTERS: GENERAL -X-RAYS: GALAXIES: CLUSTERS
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
METHODS: NUMERICAL
topic GALAXIES: CLUSTERS: GENERAL -X-RAYS: GALAXIES: CLUSTERS
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
METHODS: NUMERICAL
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 analyse the radial pressure profiles, the intracluster medium (ICM) clumping factor and the Sunyaev-Zel'dovich (SZ) scaling relations of a sample of simulated galaxy clusters and groups identified in a set of hydrodynamical simulations based on an updated version of the TREEPM-SPH GADGET-3 code. Three different sets of simulations are performed: the first assumes non-radiative physics, the others include, among other processes, active galactic nucleus (AGN) and/or stellar feedback. Our results are analysed as a function of redshift, ICM physics, cluster mass and cluster cool-coreness or dynamical state. In general, the mean pressure profiles obtained for our sample of groups and clusters show a good agreement with X-ray and SZ observations. Simulated cool-core (CC) and non-cool-core (NCC) clusters also show a good match with real data. We obtain in all cases a small (if any) redshift evolution of the pressure profiles of massive clusters, at least back to z = 1. We find that the clumpiness of gas density and pressure increases with the distance from the cluster centre and with the dynamical activity. The inclusion of AGN feedback in our simulations generates values for the gas clumping ( √ Cρ ~ 1.2 at R200) in good agreement with recent observational estimates. The simulated YSZ-Mscaling relations are in good accordance with several observed samples, especially for massive clusters. As for the scatter of these relations, we obtain a clear dependence on the cluster dynamical state, whereas this distinction is not so evident when looking at the subsamples of CC and NCC clusters.
Fil: Planelles, S.. Universidad de Valencia; España. Università degli Studi di Trieste; Italia
Fil: Fabjan, D.. Istituto Nazionale di Astrofisica; Italia. University of Ljubljana. Faculty of Mathematics and Physics; Argentina
Fil: Borgani, S.. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. University of Ljubljana. Faculty of Mathematics and Physics; Argentina
Fil: Murante, G.. Istituto Nazionale di Astrofisica; Italia
Fil: Rasia, E.. Istituto Nazionale di Astrofisica; Italia. University of Michigan; Estados Unidos
Fil: Biffi, V.. Università degli Studi di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Truong, N.. Università degli Studi di Roma Tor Vergata; Italia
Fil: Ragone Figueroa, Cinthia Judith. 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. Istituto Nazionale di Astrofisica; Italia
Fil: Granato, G. L.. Istituto Nazionale di Astrofisica; Italia
Fil: Dolag, K.. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania. University Observatory Munich; Alemania
Fil: Pierpaoli, E.. University of Southern California; Estados Unidos
Fil: Beck, A. M.. University Observatory Munich; Alemania
Fil: Steinborn, Lisa K.. University Observatory Munich; Alemania
Fil: Gaspari, M.. University of Princeton; Estados Unidos
description We analyse the radial pressure profiles, the intracluster medium (ICM) clumping factor and the Sunyaev-Zel'dovich (SZ) scaling relations of a sample of simulated galaxy clusters and groups identified in a set of hydrodynamical simulations based on an updated version of the TREEPM-SPH GADGET-3 code. Three different sets of simulations are performed: the first assumes non-radiative physics, the others include, among other processes, active galactic nucleus (AGN) and/or stellar feedback. Our results are analysed as a function of redshift, ICM physics, cluster mass and cluster cool-coreness or dynamical state. In general, the mean pressure profiles obtained for our sample of groups and clusters show a good agreement with X-ray and SZ observations. Simulated cool-core (CC) and non-cool-core (NCC) clusters also show a good match with real data. We obtain in all cases a small (if any) redshift evolution of the pressure profiles of massive clusters, at least back to z = 1. We find that the clumpiness of gas density and pressure increases with the distance from the cluster centre and with the dynamical activity. The inclusion of AGN feedback in our simulations generates values for the gas clumping ( √ Cρ ~ 1.2 at R200) in good agreement with recent observational estimates. The simulated YSZ-Mscaling relations are in good accordance with several observed samples, especially for massive clusters. As for the scatter of these relations, we obtain a clear dependence on the cluster dynamical state, whereas this distinction is not so evident when looking at the subsamples of CC and NCC clusters.
publishDate 2017
dc.date.none.fl_str_mv 2017-06
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/11336/64102
Planelles, S.; Fabjan, D.; Borgani, S.; Murante, G.; Rasia, E.; et al.; Pressure of the hot gas in simulations of galaxy clusters; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 467; 4; 6-2017; 3827-3847
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/64102
identifier_str_mv Planelles, S.; Fabjan, D.; Borgani, S.; Murante, G.; Rasia, E.; et al.; Pressure of the hot gas in simulations of galaxy clusters; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 467; 4; 6-2017; 3827-3847
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/467/4/3827/2973007
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx318
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1612.07260v1
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
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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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score 13.22299

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