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
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/273687
Ver los metadatos del registro completo
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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 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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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 |
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http://hdl.handle.net/11336/273687 |
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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 |
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eng |
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