Compact groups of galaxies in the TNG100 simulation

Autores
Celiz, Bruno Martin; Benavides, José A.; Abadi, Mario Gabriel
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Using the TNG100 cosmological simulation, we study the formation and evolution of compact groups of galaxies. Over a redshift range of 0 < z < 0.2, we identify these compact groups as Friends-of-Friends galaxy groups with a high mean surface brightness (µ_r < 26.33 mag arcsec^-2) and a minimum of four galaxy members. Typically, our compact groups have a median characteristic size of ∼150 kpc, 1D velocity dispersions of 150 km s^-1 , and stellar masses around 2 × 10^11 Msun. Roughly 1% of galaxies that have a stellar mass above 10^9 Msun lie in physically dense compact groups. We found that these systems do not constitute a separate category within the broader population of galaxy groups; instead, they represent the lower end of the size distribution in the sequence of galaxy group sizes. We traced their evolution backward in time, revealing that they initially form as galaxy systems with a mean low surface brightness that systematically increases to a peak value before stabilizing over time, exhibiting oscillatory behaviour over the following several gigayears during which mergers may occur. Mergers often transform compact groups with typically four members into galaxy pairs or triplets, which eventually can again increase their number of members by accreting a new galaxy. Nevertheless, the full merging of all constituent galaxies into a single massive galaxy is a rare phenomenon.
Fil: Celiz, Bruno Martin. 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: Benavides, José A.. University Of California At Los Angeles. Department Of Physics And Astronomy.; Estados Unidos
Fil: Abadi, Mario Gabriel. 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
GALAXIES
GROUPS
INTERACTIONS
DYNAMICS
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:11336/273687

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spelling Compact groups of galaxies in the TNG100 simulationCeliz, Bruno MartinBenavides, José A.Abadi, Mario GabrielGALAXIESGROUPSINTERACTIONSDYNAMICShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Using the TNG100 cosmological simulation, we study the formation and evolution of compact groups of galaxies. Over a redshift range of 0 < z < 0.2, we identify these compact groups as Friends-of-Friends galaxy groups with a high mean surface brightness (µ_r < 26.33 mag arcsec^-2) and a minimum of four galaxy members. Typically, our compact groups have a median characteristic size of ∼150 kpc, 1D velocity dispersions of 150 km s^-1 , and stellar masses around 2 × 10^11 Msun. Roughly 1% of galaxies that have a stellar mass above 10^9 Msun lie in physically dense compact groups. We found that these systems do not constitute a separate category within the broader population of galaxy groups; instead, they represent the lower end of the size distribution in the sequence of galaxy group sizes. We traced their evolution backward in time, revealing that they initially form as galaxy systems with a mean low surface brightness that systematically increases to a peak value before stabilizing over time, exhibiting oscillatory behaviour over the following several gigayears during which mergers may occur. Mergers often transform compact groups with typically four members into galaxy pairs or triplets, which eventually can again increase their number of members by accreting a new galaxy. Nevertheless, the full merging of all constituent galaxies into a single massive galaxy is a rare phenomenon.Fil: Celiz, Bruno Martin. 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: Benavides, José A.. University Of California At Los Angeles. Department Of Physics And Astronomy.; Estados UnidosFil: Abadi, Mario Gabriel. 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; ArgentinaEDP Sciences2025-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/273687Celiz, Bruno Martin; Benavides, José A.; Abadi, Mario Gabriel; Compact groups of galaxies in the TNG100 simulation; EDP Sciences; Astronomy and Astrophysics; 702; 9-2025; 1-110004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202555375info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202555375info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-29T12:26:41Zoai:ri.conicet.gov.ar:11336/273687instacron: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:34982025-10-29 12:26:41.688CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Compact groups of galaxies in the TNG100 simulation
title Compact groups of galaxies in the TNG100 simulation
spellingShingle Compact groups of galaxies in the TNG100 simulation
Celiz, Bruno Martin
GALAXIES
GROUPS
INTERACTIONS
DYNAMICS
title_short Compact groups of galaxies in the TNG100 simulation
title_full Compact groups of galaxies in the TNG100 simulation
title_fullStr Compact groups of galaxies in the TNG100 simulation
title_full_unstemmed Compact groups of galaxies in the TNG100 simulation
title_sort Compact groups of galaxies in the TNG100 simulation
dc.creator.none.fl_str_mv Celiz, Bruno Martin
Benavides, José A.
Abadi, Mario Gabriel
author Celiz, Bruno Martin
author_facet Celiz, Bruno Martin
Benavides, José A.
Abadi, Mario Gabriel
author_role author
author2 Benavides, José A.
Abadi, Mario Gabriel
author2_role author
author
dc.subject.none.fl_str_mv GALAXIES
GROUPS
INTERACTIONS
DYNAMICS
topic GALAXIES
GROUPS
INTERACTIONS
DYNAMICS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Using the TNG100 cosmological simulation, we study the formation and evolution of compact groups of galaxies. Over a redshift range of 0 < z < 0.2, we identify these compact groups as Friends-of-Friends galaxy groups with a high mean surface brightness (µ_r < 26.33 mag arcsec^-2) and a minimum of four galaxy members. Typically, our compact groups have a median characteristic size of ∼150 kpc, 1D velocity dispersions of 150 km s^-1 , and stellar masses around 2 × 10^11 Msun. Roughly 1% of galaxies that have a stellar mass above 10^9 Msun lie in physically dense compact groups. We found that these systems do not constitute a separate category within the broader population of galaxy groups; instead, they represent the lower end of the size distribution in the sequence of galaxy group sizes. We traced their evolution backward in time, revealing that they initially form as galaxy systems with a mean low surface brightness that systematically increases to a peak value before stabilizing over time, exhibiting oscillatory behaviour over the following several gigayears during which mergers may occur. Mergers often transform compact groups with typically four members into galaxy pairs or triplets, which eventually can again increase their number of members by accreting a new galaxy. Nevertheless, the full merging of all constituent galaxies into a single massive galaxy is a rare phenomenon.
Fil: Celiz, Bruno Martin. 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: Benavides, José A.. University Of California At Los Angeles. Department Of Physics And Astronomy.; Estados Unidos
Fil: Abadi, Mario Gabriel. 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 Using the TNG100 cosmological simulation, we study the formation and evolution of compact groups of galaxies. Over a redshift range of 0 < z < 0.2, we identify these compact groups as Friends-of-Friends galaxy groups with a high mean surface brightness (µ_r < 26.33 mag arcsec^-2) and a minimum of four galaxy members. Typically, our compact groups have a median characteristic size of ∼150 kpc, 1D velocity dispersions of 150 km s^-1 , and stellar masses around 2 × 10^11 Msun. Roughly 1% of galaxies that have a stellar mass above 10^9 Msun lie in physically dense compact groups. We found that these systems do not constitute a separate category within the broader population of galaxy groups; instead, they represent the lower end of the size distribution in the sequence of galaxy group sizes. We traced their evolution backward in time, revealing that they initially form as galaxy systems with a mean low surface brightness that systematically increases to a peak value before stabilizing over time, exhibiting oscillatory behaviour over the following several gigayears during which mergers may occur. Mergers often transform compact groups with typically four members into galaxy pairs or triplets, which eventually can again increase their number of members by accreting a new galaxy. Nevertheless, the full merging of all constituent galaxies into a single massive galaxy is a rare phenomenon.
publishDate 2025
dc.date.none.fl_str_mv 2025-09
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/11336/273687
Celiz, Bruno Martin; Benavides, José A.; Abadi, Mario Gabriel; Compact groups of galaxies in the TNG100 simulation; EDP Sciences; Astronomy and Astrophysics; 702; 9-2025; 1-11
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/273687
identifier_str_mv Celiz, Bruno Martin; Benavides, José A.; Abadi, Mario Gabriel; Compact groups of galaxies in the TNG100 simulation; EDP Sciences; Astronomy and Astrophysics; 702; 9-2025; 1-11
0004-6361
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://www.aanda.org/10.1051/0004-6361/202555375
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202555375
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 EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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