The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters

Autores
Saroon, S.; Dias, B.; Tsujimoto, T.; Parisi, Maria Celeste; Maia, F.; Kerber, L.; Bekki, K.; Minniti, D.; Oliveira, R. A. P.; Westera, P.; Katime Santrich, O. J.; Bica, E.; Sanmartim, D.; Correa Quint, B.; Fraga, L.
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (∼0.5 dex) metallicity dispersion for the SMC cluster population younger than about 7.5 Gyr, and multiple chemical evolution models tracing very different paths through the observed age–metallicity relation of the SMC. There is no doubt that these processes were complex. Therefore, a step-by-step strategy is required in order to better understand the SMC chemical evolution. We adopted an existing framework to split the SMC intoregions on the sky, and we focus on the west halo in this work, which contains the oldest and most metal-poor stellar populations and is moving away from the SMC, that is, in an opposite motion with respect to the Magellanic Bridge. We present a sample containing ∼60% of all west halo clusters to represent the region well, and we identify a clear age–metallicity relation with a tight dispersionthat exhibits a 0.5 dex metallicity dip about 6 Gyr ago. We ran chemical evolution models and discuss possible scenarios to explain this metallicity dip, the most likely being a major merger accelerating the SFR after the event. This merger should be combined with inefficient internal gas mixing within the SMC and different SFRs in different SMC regions because the same metallicity dip is not seen in the AMR of the SMC combining clusters from all regions. We try to explain the scenario to better understand the SMC chemo-dynamical history.
Fil: Saroon, S.. Universidad Andrés Bello; Chile
Fil: Dias, B.. Universidad de Tarapacá; Chile
Fil: Tsujimoto, T.. National Astronomical Observatory Of Japan; Japón
Fil: Parisi, Maria Celeste. 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: Maia, F.. Universidade Federal do Rio de Janeiro; Brasil
Fil: Kerber, L.. Universidade Estadual de Santa Cruz; Brasil
Fil: Bekki, K.. University of Western Australia; Australia
Fil: Minniti, D.. Universidad Andrés Bello; Chile
Fil: Oliveira, R. A. P.. Universidade de Sao Paulo; Brasil
Fil: Westera, P.. Universidad Federal Do Abc; Brasil
Fil: Katime Santrich, O. J.. Universidade Estadual de Santa Cruz; Brasil
Fil: Bica, E.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Sanmartim, D.. Rubin Observatory Project Office; Estados Unidos
Fil: Correa Quint, B.. Rubin Observatory Project Office; Estados Unidos
Fil: Fraga, L.. Laboratório Nacional de Astrofísica; Brasil
Materia
GALAXIES: DWARF
GALACIES: INTERACTIONS
MAGELLANIC CLOUDS
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:11336/231603
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/231603
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clustersSaroon, S.Dias, B.Tsujimoto, T.Parisi, Maria CelesteMaia, F.Kerber, L.Bekki, K.Minniti, D.Oliveira, R. A. P.Westera, P.Katime Santrich, O. J.Bica, E.Sanmartim, D.Correa Quint, B.Fraga, L.GALAXIES: DWARFGALACIES: INTERACTIONSMAGELLANIC CLOUDSGALAXIES: CLUSTERS: GENERALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (∼0.5 dex) metallicity dispersion for the SMC cluster population younger than about 7.5 Gyr, and multiple chemical evolution models tracing very different paths through the observed age–metallicity relation of the SMC. There is no doubt that these processes were complex. Therefore, a step-by-step strategy is required in order to better understand the SMC chemical evolution. We adopted an existing framework to split the SMC intoregions on the sky, and we focus on the west halo in this work, which contains the oldest and most metal-poor stellar populations and is moving away from the SMC, that is, in an opposite motion with respect to the Magellanic Bridge. We present a sample containing ∼60% of all west halo clusters to represent the region well, and we identify a clear age–metallicity relation with a tight dispersionthat exhibits a 0.5 dex metallicity dip about 6 Gyr ago. We ran chemical evolution models and discuss possible scenarios to explain this metallicity dip, the most likely being a major merger accelerating the SFR after the event. This merger should be combined with inefficient internal gas mixing within the SMC and different SFRs in different SMC regions because the same metallicity dip is not seen in the AMR of the SMC combining clusters from all regions. We try to explain the scenario to better understand the SMC chemo-dynamical history.Fil: Saroon, S.. Universidad Andrés Bello; ChileFil: Dias, B.. Universidad de Tarapacá; ChileFil: Tsujimoto, T.. National Astronomical Observatory Of Japan; JapónFil: Parisi, Maria Celeste. 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: Maia, F.. Universidade Federal do Rio de Janeiro; BrasilFil: Kerber, L.. Universidade Estadual de Santa Cruz; BrasilFil: Bekki, K.. University of Western Australia; AustraliaFil: Minniti, D.. Universidad Andrés Bello; ChileFil: Oliveira, R. A. P.. Universidade de Sao Paulo; BrasilFil: Westera, P.. Universidad Federal Do Abc; BrasilFil: Katime Santrich, O. J.. Universidade Estadual de Santa Cruz; BrasilFil: Bica, E.. Universidade Federal do Rio Grande do Sul; BrasilFil: Sanmartim, D.. Rubin Observatory Project Office; Estados UnidosFil: Correa Quint, B.. Rubin Observatory Project Office; Estados UnidosFil: Fraga, L.. Laboratório Nacional de Astrofísica; BrasilEDP Sciences2023-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/231603Saroon, S.; Dias, B.; Tsujimoto, T.; Parisi, Maria Celeste; Maia, F.; et al.; The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters; EDP Sciences; Astronomy and Astrophysics; 677; 9-20231432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2023/09/aa46648-23/aa46648-23.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202346648info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:40:14Zoai:ri.conicet.gov.ar:11336/231603instacron: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 09:40:14.613CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
title The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
spellingShingle The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
Saroon, S.
GALAXIES: DWARF
GALACIES: INTERACTIONS
MAGELLANIC CLOUDS
GALAXIES: CLUSTERS: GENERAL
title_short The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
title_full The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
title_fullStr The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
title_full_unstemmed The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
title_sort The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters
dc.creator.none.fl_str_mv Saroon, S.
Dias, B.
Tsujimoto, T.
Parisi, Maria Celeste
Maia, F.
Kerber, L.
Bekki, K.
Minniti, D.
Oliveira, R. A. P.
Westera, P.
Katime Santrich, O. J.
Bica, E.
Sanmartim, D.
Correa Quint, B.
Fraga, L.
author Saroon, S.
author_facet Saroon, S.
Dias, B.
Tsujimoto, T.
Parisi, Maria Celeste
Maia, F.
Kerber, L.
Bekki, K.
Minniti, D.
Oliveira, R. A. P.
Westera, P.
Katime Santrich, O. J.
Bica, E.
Sanmartim, D.
Correa Quint, B.
Fraga, L.
author_role author
author2 Dias, B.
Tsujimoto, T.
Parisi, Maria Celeste
Maia, F.
Kerber, L.
Bekki, K.
Minniti, D.
Oliveira, R. A. P.
Westera, P.
Katime Santrich, O. J.
Bica, E.
Sanmartim, D.
Correa Quint, B.
Fraga, L.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: DWARF
GALACIES: INTERACTIONS
MAGELLANIC CLOUDS
GALAXIES: CLUSTERS: GENERAL
topic GALAXIES: DWARF
GALACIES: INTERACTIONS
MAGELLANIC CLOUDS
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 The chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (∼0.5 dex) metallicity dispersion for the SMC cluster population younger than about 7.5 Gyr, and multiple chemical evolution models tracing very different paths through the observed age–metallicity relation of the SMC. There is no doubt that these processes were complex. Therefore, a step-by-step strategy is required in order to better understand the SMC chemical evolution. We adopted an existing framework to split the SMC intoregions on the sky, and we focus on the west halo in this work, which contains the oldest and most metal-poor stellar populations and is moving away from the SMC, that is, in an opposite motion with respect to the Magellanic Bridge. We present a sample containing ∼60% of all west halo clusters to represent the region well, and we identify a clear age–metallicity relation with a tight dispersionthat exhibits a 0.5 dex metallicity dip about 6 Gyr ago. We ran chemical evolution models and discuss possible scenarios to explain this metallicity dip, the most likely being a major merger accelerating the SFR after the event. This merger should be combined with inefficient internal gas mixing within the SMC and different SFRs in different SMC regions because the same metallicity dip is not seen in the AMR of the SMC combining clusters from all regions. We try to explain the scenario to better understand the SMC chemo-dynamical history.
Fil: Saroon, S.. Universidad Andrés Bello; Chile
Fil: Dias, B.. Universidad de Tarapacá; Chile
Fil: Tsujimoto, T.. National Astronomical Observatory Of Japan; Japón
Fil: Parisi, Maria Celeste. 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: Maia, F.. Universidade Federal do Rio de Janeiro; Brasil
Fil: Kerber, L.. Universidade Estadual de Santa Cruz; Brasil
Fil: Bekki, K.. University of Western Australia; Australia
Fil: Minniti, D.. Universidad Andrés Bello; Chile
Fil: Oliveira, R. A. P.. Universidade de Sao Paulo; Brasil
Fil: Westera, P.. Universidad Federal Do Abc; Brasil
Fil: Katime Santrich, O. J.. Universidade Estadual de Santa Cruz; Brasil
Fil: Bica, E.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Sanmartim, D.. Rubin Observatory Project Office; Estados Unidos
Fil: Correa Quint, B.. Rubin Observatory Project Office; Estados Unidos
Fil: Fraga, L.. Laboratório Nacional de Astrofísica; Brasil
description The chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (∼0.5 dex) metallicity dispersion for the SMC cluster population younger than about 7.5 Gyr, and multiple chemical evolution models tracing very different paths through the observed age–metallicity relation of the SMC. There is no doubt that these processes were complex. Therefore, a step-by-step strategy is required in order to better understand the SMC chemical evolution. We adopted an existing framework to split the SMC intoregions on the sky, and we focus on the west halo in this work, which contains the oldest and most metal-poor stellar populations and is moving away from the SMC, that is, in an opposite motion with respect to the Magellanic Bridge. We present a sample containing ∼60% of all west halo clusters to represent the region well, and we identify a clear age–metallicity relation with a tight dispersionthat exhibits a 0.5 dex metallicity dip about 6 Gyr ago. We ran chemical evolution models and discuss possible scenarios to explain this metallicity dip, the most likely being a major merger accelerating the SFR after the event. This merger should be combined with inefficient internal gas mixing within the SMC and different SFRs in different SMC regions because the same metallicity dip is not seen in the AMR of the SMC combining clusters from all regions. We try to explain the scenario to better understand the SMC chemo-dynamical history.
publishDate 2023
dc.date.none.fl_str_mv 2023-09
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/11336/231603
Saroon, S.; Dias, B.; Tsujimoto, T.; Parisi, Maria Celeste; Maia, F.; et al.; The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters; EDP Sciences; Astronomy and Astrophysics; 677; 9-2023
1432-0746
CONICET Digital
CONICET
url http://hdl.handle.net/11336/231603
identifier_str_mv Saroon, S.; Dias, B.; Tsujimoto, T.; Parisi, Maria Celeste; Maia, F.; et al.; The VISCACHA survey. VIII. Chemical evolution history of the Small Magellanic Cloud west halo clusters; EDP Sciences; Astronomy and Astrophysics; 677; 9-2023
1432-0746
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/articles/aa/full_html/2023/09/aa46648-23/aa46648-23.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202346648
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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score 13.070432

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