Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies

Autores
Pallero, Diego; Gómez, Facundo Ariel; Padilla, Nelson David; Bahé, Yannick M; Vega Martínez, Cristian Antonio; Torres Flores, S.
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 (80 per cent ) reached this state in a dense environment (log 10 M 200 [M] ?13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low-mass clusters. Moreo v er, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster's r 200 they rapidly become quenched (1 Gyr). Just a small fraction of galaxies (15 per cent ) is capable of retaining their gas for a longer period of time, but after 4 Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ?ICM ?3 ×10 ?5 n H (cm ?3 ). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r 200 and that, by the time they reach r 500 , most of them are already quenched
Fil: Pallero, Diego. Universidad de La Serena; Chile. Universidad de Valparaíso; Chile
Fil: Gómez, Facundo Ariel. Universidad de La Serena; Chile
Fil: Padilla, Nelson David. Universidad Católica de Chile; Chile. Pontificia Universidad Católica de Chile; Chile. 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: Bahé, Yannick M. Sterrewacht Leiden; Alemania
Fil: Vega Martínez, Cristian Antonio. Universidad de La Serena; Chile. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Torres Flores, S.. Universidad de La Serena; Chile
Materia
GALAXIES: EVOLUTION
GALAXIES: FORMATION
GALAXIES: HALOES
GALAXIES: STAR FORMATION
GALAXIES:CLUSTERS: 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:11336/202898
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/202898
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxiesPallero, DiegoGómez, Facundo ArielPadilla, Nelson DavidBahé, Yannick MVega Martínez, Cristian AntonioTorres Flores, S.GALAXIES: EVOLUTIONGALAXIES: FORMATIONGALAXIES: HALOESGALAXIES: STAR FORMATIONGALAXIES:CLUSTERS: GENERALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 (80 per cent ) reached this state in a dense environment (log 10 M 200 [M] ?13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low-mass clusters. Moreo v er, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster's r 200 they rapidly become quenched (1 Gyr). Just a small fraction of galaxies (15 per cent ) is capable of retaining their gas for a longer period of time, but after 4 Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ?ICM ?3 ×10 ?5 n H (cm ?3 ). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r 200 and that, by the time they reach r 500 , most of them are already quenchedFil: Pallero, Diego. Universidad de La Serena; Chile. Universidad de Valparaíso; ChileFil: Gómez, Facundo Ariel. Universidad de La Serena; ChileFil: Padilla, Nelson David. Universidad Católica de Chile; Chile. Pontificia Universidad Católica de Chile; Chile. 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: Bahé, Yannick M. Sterrewacht Leiden; AlemaniaFil: Vega Martínez, Cristian Antonio. Universidad de La Serena; Chile. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Torres Flores, S.. Universidad de La Serena; ChileOxford University Press2022-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/202898Pallero, Diego; Gómez, Facundo Ariel; Padilla, Nelson David; Bahé, Yannick M; Vega Martínez, Cristian Antonio; et al.; Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 511; 3; 4-2022; 3210-32270035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stab3318info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/511/3/3210/6430177?redirectedFrom=fulltextinfo:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2012.08593info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:36:15Zoai:ri.conicet.gov.ar:11336/202898instacron: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 09:36:15.775CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
title Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
spellingShingle Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
Pallero, Diego
GALAXIES: EVOLUTION
GALAXIES: FORMATION
GALAXIES: HALOES
GALAXIES: STAR FORMATION
GALAXIES:CLUSTERS: GENERAL
title_short Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
title_full Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
title_fullStr Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
title_full_unstemmed Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
title_sort Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies
dc.creator.none.fl_str_mv Pallero, Diego
Gómez, Facundo Ariel
Padilla, Nelson David
Bahé, Yannick M
Vega Martínez, Cristian Antonio
Torres Flores, S.
author Pallero, Diego
author_facet Pallero, Diego
Gómez, Facundo Ariel
Padilla, Nelson David
Bahé, Yannick M
Vega Martínez, Cristian Antonio
Torres Flores, S.
author_role author
author2 Gómez, Facundo Ariel
Padilla, Nelson David
Bahé, Yannick M
Vega Martínez, Cristian Antonio
Torres Flores, S.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: EVOLUTION
GALAXIES: FORMATION
GALAXIES: HALOES
GALAXIES: STAR FORMATION
GALAXIES:CLUSTERS: GENERAL
topic GALAXIES: EVOLUTION
GALAXIES: FORMATION
GALAXIES: HALOES
GALAXIES: STAR FORMATION
GALAXIES:CLUSTERS: 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 study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 (80 per cent ) reached this state in a dense environment (log 10 M 200 [M] ?13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low-mass clusters. Moreo v er, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster's r 200 they rapidly become quenched (1 Gyr). Just a small fraction of galaxies (15 per cent ) is capable of retaining their gas for a longer period of time, but after 4 Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ?ICM ?3 ×10 ?5 n H (cm ?3 ). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r 200 and that, by the time they reach r 500 , most of them are already quenched
Fil: Pallero, Diego. Universidad de La Serena; Chile. Universidad de Valparaíso; Chile
Fil: Gómez, Facundo Ariel. Universidad de La Serena; Chile
Fil: Padilla, Nelson David. Universidad Católica de Chile; Chile. Pontificia Universidad Católica de Chile; Chile. 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: Bahé, Yannick M. Sterrewacht Leiden; Alemania
Fil: Vega Martínez, Cristian Antonio. Universidad de La Serena; Chile. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Torres Flores, S.. Universidad de La Serena; Chile
description We study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 (80 per cent ) reached this state in a dense environment (log 10 M 200 [M] ?13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low-mass clusters. Moreo v er, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster's r 200 they rapidly become quenched (1 Gyr). Just a small fraction of galaxies (15 per cent ) is capable of retaining their gas for a longer period of time, but after 4 Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ?ICM ?3 ×10 ?5 n H (cm ?3 ). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r 200 and that, by the time they reach r 500 , most of them are already quenched
publishDate 2022
dc.date.none.fl_str_mv 2022-04
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/11336/202898
Pallero, Diego; Gómez, Facundo Ariel; Padilla, Nelson David; Bahé, Yannick M; Vega Martínez, Cristian Antonio; et al.; Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 511; 3; 4-2022; 3210-3227
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/202898
identifier_str_mv Pallero, Diego; Gómez, Facundo Ariel; Padilla, Nelson David; Bahé, Yannick M; Vega Martínez, Cristian Antonio; et al.; Too dense to go through: The role of low-mass clusters in the pre-processing of satellite galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 511; 3; 4-2022; 3210-3227
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stab3318
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/511/3/3210/6430177?redirectedFrom=fulltext
info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2012.08593
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 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 13.070432

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