Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud

Autores
Geisler, Doug; Piatti, Andres Eduardo; Bica, E.; Claria Olmedo, Juan Jose
Año de publicación
2003
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present Eashington system colour-magnitude diagramsfor 8 stars clusters and their surrounding fields which, with one exception, lie within the inner parts of the Large Magellanic Cloud (LMC) disc. Careful attention is paid to separating out the cluster and field star distributions. Ages and metallicities are then determined in a consistent manner for both populations in two different ways. We first compare the colour-magnitude diagrams (CMDs) with new theoretical isochrones in the Washington system. We also derive ages using the magnitude difference between the red clump and the turnoff, and derive metallicities by comparing the giant branches to standard calibrating clusters. For this latter mtallcitiy derivation, we present age-cdependent metallicity corrections for intermediate age clusters (IACs) based on the new isochrones. The two methods for both age and metallicity determination are in good agreement with each other. All clusters are found to be IACs 1-3 Gyr), with metallicities from -0.4 to -0.9. We find that the stellar population of each star cluster is generally quite similar to that of the field where it is embedded, sharing its mean age and metallicity. Combining the present sample with a revision of of Bica et al.. studied similarly, we find that our metallicities for IACs are intermediate in metallicity to those for clusters of similar age studied by Olsewski et al. and Beasley, Hoyle & Sharples. A combined age-metallicity relation is presented which shows that LMC clusters formed between 1-3 Gyr ago with a mean metallicity (-0.5 dex) and metallicity spread (0.23 dex) independent of age. Good agreement is found with the bursting model of pagel & Tautvaisiene. No evidence for a metallicity gradient is found.   
Fil: Geisler, Doug. Universidad de Concepción; Chile
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Bica, E.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Claria Olmedo, Juan Jose. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Materia
Star cluster
Photometry
Large Magellanic Cloud
Metallicity
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:11336/22341
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/22341
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic CloudGeisler, DougPiatti, Andres EduardoBica, E.Claria Olmedo, Juan JoseStar clusterPhotometryLarge Magellanic CloudMetallicityhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present Eashington system colour-magnitude diagramsfor 8 stars clusters and their surrounding fields which, with one exception, lie within the inner parts of the Large Magellanic Cloud (LMC) disc. Careful attention is paid to separating out the cluster and field star distributions. Ages and metallicities are then determined in a consistent manner for both populations in two different ways. We first compare the colour-magnitude diagrams (CMDs) with new theoretical isochrones in the Washington system. We also derive ages using the magnitude difference between the red clump and the turnoff, and derive metallicities by comparing the giant branches to standard calibrating clusters. For this latter mtallcitiy derivation, we present age-cdependent metallicity corrections for intermediate age clusters (IACs) based on the new isochrones. The two methods for both age and metallicity determination are in good agreement with each other. All clusters are found to be IACs 1-3 Gyr), with metallicities from -0.4 to -0.9. We find that the stellar population of each star cluster is generally quite similar to that of the field where it is embedded, sharing its mean age and metallicity. Combining the present sample with a revision of of Bica et al.. studied similarly, we find that our metallicities for IACs are intermediate in metallicity to those for clusters of similar age studied by Olsewski et al. and Beasley, Hoyle & Sharples. A combined age-metallicity relation is presented which shows that LMC clusters formed between 1-3 Gyr ago with a mean metallicity (-0.5 dex) and metallicity spread (0.23 dex) independent of age. Good agreement is found with the bursting model of pagel & Tautvaisiene. No evidence for a metallicity gradient is found.   Fil: Geisler, Doug. Universidad de Concepción; ChileFil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Bica, E.. Universidade Federal do Rio Grande do Sul; BrasilFil: Claria Olmedo, Juan Jose. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaOxford University Press2003-05info: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/11336/22341Geisler, Doug; Piatti, Andres Eduardo; Bica, E.; Claria Olmedo, Juan Jose; Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 341; 3; 5-2003; 771-7840035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1046/j.1365-8711.2003.06408.xinfo:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2003.06408.xinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:24:43Zoai:ri.conicet.gov.ar:11336/22341instacron: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:34982025-10-22 11:24:43.67CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
title Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
spellingShingle Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
Geisler, Doug
Star cluster
Photometry
Large Magellanic Cloud
Metallicity
title_short Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
title_full Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
title_fullStr Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
title_full_unstemmed Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
title_sort Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud
dc.creator.none.fl_str_mv Geisler, Doug
Piatti, Andres Eduardo
Bica, E.
Claria Olmedo, Juan Jose
author Geisler, Doug
author_facet Geisler, Doug
Piatti, Andres Eduardo
Bica, E.
Claria Olmedo, Juan Jose
author_role author
author2 Piatti, Andres Eduardo
Bica, E.
Claria Olmedo, Juan Jose
author2_role author
author
author
dc.subject.none.fl_str_mv Star cluster
Photometry
Large Magellanic Cloud
Metallicity
topic Star cluster
Photometry
Large Magellanic Cloud
Metallicity
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 present Eashington system colour-magnitude diagramsfor 8 stars clusters and their surrounding fields which, with one exception, lie within the inner parts of the Large Magellanic Cloud (LMC) disc. Careful attention is paid to separating out the cluster and field star distributions. Ages and metallicities are then determined in a consistent manner for both populations in two different ways. We first compare the colour-magnitude diagrams (CMDs) with new theoretical isochrones in the Washington system. We also derive ages using the magnitude difference between the red clump and the turnoff, and derive metallicities by comparing the giant branches to standard calibrating clusters. For this latter mtallcitiy derivation, we present age-cdependent metallicity corrections for intermediate age clusters (IACs) based on the new isochrones. The two methods for both age and metallicity determination are in good agreement with each other. All clusters are found to be IACs 1-3 Gyr), with metallicities from -0.4 to -0.9. We find that the stellar population of each star cluster is generally quite similar to that of the field where it is embedded, sharing its mean age and metallicity. Combining the present sample with a revision of of Bica et al.. studied similarly, we find that our metallicities for IACs are intermediate in metallicity to those for clusters of similar age studied by Olsewski et al. and Beasley, Hoyle & Sharples. A combined age-metallicity relation is presented which shows that LMC clusters formed between 1-3 Gyr ago with a mean metallicity (-0.5 dex) and metallicity spread (0.23 dex) independent of age. Good agreement is found with the bursting model of pagel & Tautvaisiene. No evidence for a metallicity gradient is found.   
Fil: Geisler, Doug. Universidad de Concepción; Chile
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Bica, E.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Claria Olmedo, Juan Jose. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
description We present Eashington system colour-magnitude diagramsfor 8 stars clusters and their surrounding fields which, with one exception, lie within the inner parts of the Large Magellanic Cloud (LMC) disc. Careful attention is paid to separating out the cluster and field star distributions. Ages and metallicities are then determined in a consistent manner for both populations in two different ways. We first compare the colour-magnitude diagrams (CMDs) with new theoretical isochrones in the Washington system. We also derive ages using the magnitude difference between the red clump and the turnoff, and derive metallicities by comparing the giant branches to standard calibrating clusters. For this latter mtallcitiy derivation, we present age-cdependent metallicity corrections for intermediate age clusters (IACs) based on the new isochrones. The two methods for both age and metallicity determination are in good agreement with each other. All clusters are found to be IACs 1-3 Gyr), with metallicities from -0.4 to -0.9. We find that the stellar population of each star cluster is generally quite similar to that of the field where it is embedded, sharing its mean age and metallicity. Combining the present sample with a revision of of Bica et al.. studied similarly, we find that our metallicities for IACs are intermediate in metallicity to those for clusters of similar age studied by Olsewski et al. and Beasley, Hoyle & Sharples. A combined age-metallicity relation is presented which shows that LMC clusters formed between 1-3 Gyr ago with a mean metallicity (-0.5 dex) and metallicity spread (0.23 dex) independent of age. Good agreement is found with the bursting model of pagel & Tautvaisiene. No evidence for a metallicity gradient is found.   
publishDate 2003
dc.date.none.fl_str_mv 2003-05
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/11336/22341
Geisler, Doug; Piatti, Andres Eduardo; Bica, E.; Claria Olmedo, Juan Jose; Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 341; 3; 5-2003; 771-784
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/22341
identifier_str_mv Geisler, Doug; Piatti, Andres Eduardo; Bica, E.; Claria Olmedo, Juan Jose; Ages and metallicities of eight star clusters and their surrounding fields in the inner disc of the Large Magellanic Cloud; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 341; 3; 5-2003; 771-784
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/url/https://academic.oup.com/mnras/article-lookup/doi/10.1046/j.1365-8711.2003.06408.x
info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2003.06408.x
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 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 12.982451

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