BCG mass evolution in cosmological hydro-simulations

Autores
Ragone Figueroa, Cinthia Judith; Granato, Gian Luigi; Ferraro, María Eugenia; Murante, G.; Biffi, V.; Borgani, S.; Planelles, S.; Rasia, E.
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We analyze the stellar growth of brightest cluster galaxies (BCGs) produced by cosmological zoom-in hydrodynamical simulations of the formation of massive galaxy clusters. The evolution of the stellar mass content is studied considering different apertures, and tracking backwards either the main progenitor of the z = 0 BCG or that of the cluster hosting the BCG at z = 0. Both methods lead to similar results up to z ≃ 1.5. The simulated BCG masses at z = 0 are in agreement with recent observations. In the redshift interval from z = 1 to 0, we find growth factors 1.3, 1.6 and 3.6 for stellar masses within 30 kpc, 50 kpc and 10 per cent of R500, respectively. The first two factors, and, in general, the mass evolution in this redshift range, are in agreement with most recent observations. The last larger factor is similar to the growth factor obtained by a semi-analytical model (SAM). Half of the star particles that end up in the inner 50 kpc was typically formed by redshift ~3.7, while the assembly of half of the BCGs stellar mass occurs on average at lower redshifts ~1.5. This assembly redshift correlates with the mass attained by the cluster at high z ≳ 1.3, due to the broader range of the progenitor clusters at high-z. The assembly redshift of BCGs decreases with increasing apertures. Our results are compatible with the inside-out scenario. Simulated BCGs could lack intense enough star formation (SF) at high redshift, while possibly exhibit an excess of residual SF at low redshift.
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
Fil: Granato, Gian Luigi. Osservatorio Astronomico Di Trieste;
Fil: Ferraro, María Eugenia. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Murante, G.. Osservatorio Astronomico di Trieste; Italia
Fil: Biffi, V.. Osservatorio Astronomico di Trieste; Italia
Fil: Borgani, S.. Instituto de Astronomia Teorica y Experimental; Argentina. Osservatorio Astronomico di Trieste; Italia
Fil: Planelles, S.. Universidad de Valencia; España
Fil: Rasia, E.. Università degli Studi di Trieste; Italia
Materia
CD- GALAXIES: EVOLUTION
GALAXIES: ELLIPTICAL AND LENTICULAR
GALAXIES: FORMATION
GALAXIES: HALOES
METHODS: NUMERICAL
QUASARS: GENERAL
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:11336/89512
Acceder
id CONICETDig_f1da1a73d0355f367c9ec196d5670eb3
oai_identifier_str oai:ri.conicet.gov.ar:11336/89512
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling BCG mass evolution in cosmological hydro-simulationsRagone Figueroa, Cinthia JudithGranato, Gian LuigiFerraro, María EugeniaMurante, G.Biffi, V.Borgani, S.Planelles, S.Rasia, E.CD- GALAXIES: EVOLUTIONGALAXIES: ELLIPTICAL AND LENTICULARGALAXIES: FORMATIONGALAXIES: HALOESMETHODS: NUMERICALQUASARS: GENERALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We analyze the stellar growth of brightest cluster galaxies (BCGs) produced by cosmological zoom-in hydrodynamical simulations of the formation of massive galaxy clusters. The evolution of the stellar mass content is studied considering different apertures, and tracking backwards either the main progenitor of the z = 0 BCG or that of the cluster hosting the BCG at z = 0. Both methods lead to similar results up to z ≃ 1.5. The simulated BCG masses at z = 0 are in agreement with recent observations. In the redshift interval from z = 1 to 0, we find growth factors 1.3, 1.6 and 3.6 for stellar masses within 30 kpc, 50 kpc and 10 per cent of R500, respectively. The first two factors, and, in general, the mass evolution in this redshift range, are in agreement with most recent observations. The last larger factor is similar to the growth factor obtained by a semi-analytical model (SAM). Half of the star particles that end up in the inner 50 kpc was typically formed by redshift ~3.7, while the assembly of half of the BCGs stellar mass occurs on average at lower redshifts ~1.5. This assembly redshift correlates with the mass attained by the cluster at high z ≳ 1.3, due to the broader range of the progenitor clusters at high-z. The assembly redshift of BCGs decreases with increasing apertures. Our results are compatible with the inside-out scenario. Simulated BCGs could lack intense enough star formation (SF) at high redshift, while possibly exhibit an excess of residual SF at low redshift.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; ArgentinaFil: Granato, Gian Luigi. Osservatorio Astronomico Di Trieste;Fil: Ferraro, María Eugenia. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Murante, G.. Osservatorio Astronomico di Trieste; ItaliaFil: Biffi, V.. Osservatorio Astronomico di Trieste; ItaliaFil: Borgani, S.. Instituto de Astronomia Teorica y Experimental; Argentina. Osservatorio Astronomico di Trieste; ItaliaFil: Planelles, S.. Universidad de Valencia; EspañaFil: Rasia, E.. Università degli Studi di Trieste; ItaliaWiley Blackwell Publishing, Inc2018-09info: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/11336/89512Ragone Figueroa, Cinthia Judith; Granato, Gian Luigi; Ferraro, María Eugenia; Murante, G.; Biffi, V.; et al.; BCG mass evolution in cosmological hydro-simulations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 1; 9-2018; 1125-11360035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2018MNRAS.479.1125Rinfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1639info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:29:28Zoai:ri.conicet.gov.ar:11336/89512instacron: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 10:29:28.958CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv BCG mass evolution in cosmological hydro-simulations
title BCG mass evolution in cosmological hydro-simulations
spellingShingle BCG mass evolution in cosmological hydro-simulations
Ragone Figueroa, Cinthia Judith
CD- GALAXIES: EVOLUTION
GALAXIES: ELLIPTICAL AND LENTICULAR
GALAXIES: FORMATION
GALAXIES: HALOES
METHODS: NUMERICAL
QUASARS: GENERAL
title_short BCG mass evolution in cosmological hydro-simulations
title_full BCG mass evolution in cosmological hydro-simulations
title_fullStr BCG mass evolution in cosmological hydro-simulations
title_full_unstemmed BCG mass evolution in cosmological hydro-simulations
title_sort BCG mass evolution in cosmological hydro-simulations
dc.creator.none.fl_str_mv Ragone Figueroa, Cinthia Judith
Granato, Gian Luigi
Ferraro, María Eugenia
Murante, G.
Biffi, V.
Borgani, S.
Planelles, S.
Rasia, E.
author Ragone Figueroa, Cinthia Judith
author_facet Ragone Figueroa, Cinthia Judith
Granato, Gian Luigi
Ferraro, María Eugenia
Murante, G.
Biffi, V.
Borgani, S.
Planelles, S.
Rasia, E.
author_role author
author2 Granato, Gian Luigi
Ferraro, María Eugenia
Murante, G.
Biffi, V.
Borgani, S.
Planelles, S.
Rasia, E.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv CD- GALAXIES: EVOLUTION
GALAXIES: ELLIPTICAL AND LENTICULAR
GALAXIES: FORMATION
GALAXIES: HALOES
METHODS: NUMERICAL
QUASARS: GENERAL
topic CD- GALAXIES: EVOLUTION
GALAXIES: ELLIPTICAL AND LENTICULAR
GALAXIES: FORMATION
GALAXIES: HALOES
METHODS: NUMERICAL
QUASARS: GENERAL
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 analyze the stellar growth of brightest cluster galaxies (BCGs) produced by cosmological zoom-in hydrodynamical simulations of the formation of massive galaxy clusters. The evolution of the stellar mass content is studied considering different apertures, and tracking backwards either the main progenitor of the z = 0 BCG or that of the cluster hosting the BCG at z = 0. Both methods lead to similar results up to z ≃ 1.5. The simulated BCG masses at z = 0 are in agreement with recent observations. In the redshift interval from z = 1 to 0, we find growth factors 1.3, 1.6 and 3.6 for stellar masses within 30 kpc, 50 kpc and 10 per cent of R500, respectively. The first two factors, and, in general, the mass evolution in this redshift range, are in agreement with most recent observations. The last larger factor is similar to the growth factor obtained by a semi-analytical model (SAM). Half of the star particles that end up in the inner 50 kpc was typically formed by redshift ~3.7, while the assembly of half of the BCGs stellar mass occurs on average at lower redshifts ~1.5. This assembly redshift correlates with the mass attained by the cluster at high z ≳ 1.3, due to the broader range of the progenitor clusters at high-z. The assembly redshift of BCGs decreases with increasing apertures. Our results are compatible with the inside-out scenario. Simulated BCGs could lack intense enough star formation (SF) at high redshift, while possibly exhibit an excess of residual SF at low redshift.
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
Fil: Granato, Gian Luigi. Osservatorio Astronomico Di Trieste;
Fil: Ferraro, María Eugenia. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Murante, G.. Osservatorio Astronomico di Trieste; Italia
Fil: Biffi, V.. Osservatorio Astronomico di Trieste; Italia
Fil: Borgani, S.. Instituto de Astronomia Teorica y Experimental; Argentina. Osservatorio Astronomico di Trieste; Italia
Fil: Planelles, S.. Universidad de Valencia; España
Fil: Rasia, E.. Università degli Studi di Trieste; Italia
description We analyze the stellar growth of brightest cluster galaxies (BCGs) produced by cosmological zoom-in hydrodynamical simulations of the formation of massive galaxy clusters. The evolution of the stellar mass content is studied considering different apertures, and tracking backwards either the main progenitor of the z = 0 BCG or that of the cluster hosting the BCG at z = 0. Both methods lead to similar results up to z ≃ 1.5. The simulated BCG masses at z = 0 are in agreement with recent observations. In the redshift interval from z = 1 to 0, we find growth factors 1.3, 1.6 and 3.6 for stellar masses within 30 kpc, 50 kpc and 10 per cent of R500, respectively. The first two factors, and, in general, the mass evolution in this redshift range, are in agreement with most recent observations. The last larger factor is similar to the growth factor obtained by a semi-analytical model (SAM). Half of the star particles that end up in the inner 50 kpc was typically formed by redshift ~3.7, while the assembly of half of the BCGs stellar mass occurs on average at lower redshifts ~1.5. This assembly redshift correlates with the mass attained by the cluster at high z ≳ 1.3, due to the broader range of the progenitor clusters at high-z. The assembly redshift of BCGs decreases with increasing apertures. Our results are compatible with the inside-out scenario. Simulated BCGs could lack intense enough star formation (SF) at high redshift, while possibly exhibit an excess of residual SF at low redshift.
publishDate 2018
dc.date.none.fl_str_mv 2018-09
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/11336/89512
Ragone Figueroa, Cinthia Judith; Granato, Gian Luigi; Ferraro, María Eugenia; Murante, G.; Biffi, V.; et al.; BCG mass evolution in cosmological hydro-simulations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 1; 9-2018; 1125-1136
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/89512
identifier_str_mv Ragone Figueroa, Cinthia Judith; Granato, Gian Luigi; Ferraro, María Eugenia; Murante, G.; Biffi, V.; et al.; BCG mass evolution in cosmological hydro-simulations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 1; 9-2018; 1125-1136
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/2018MNRAS.479.1125R
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1639
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 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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score 13.070432

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