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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/22341
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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 Técnicas2025-09-29T09:55:36Zoai: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:34982025-09-29 09:55:37.086CONICET 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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1844613675866914816 |
score |
13.070432 |