Seven young star clusters in the inner region of the Small Magellanic Cloud

Autores
Piatti, Andres Eduardo; Geisler, Doug; Sarajedini, Ata; Gallart, Carme; Wischnjewsky, Marina
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present CCD photometry in the Washington system C and T1 passbands down to T1∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T1 magnitudes and C−T1 colours for a total of 114 826 stars distributed throughout cluster areas of 13.7 × 13.7 arcmin2 each. Cluster radii were estimated from star counts distributed throughout the entire observed fields. The seven clusters are generally characterized by a relatively small angular size and by a high field star contamination. We performed an in-depth analysis of the field star contamination of the colour–magnitude diagrams (CMDs), and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T1, C−T1) CMDs, we derive ages for the sample, assuming Z= 0.004, finding ages between 25 Myr and 1.2 Gyr. We then examined different relationships between positions in the SMC, age and metallicity of a larger sample of clusters including our previous work whose ages and metallicities are on the same scale used in this paper. We confirm previous results in the sense that the further a cluster is from the centre of the galaxy, the older and more metal poor it is, with some dispersion; although clusters associated with the Magellanic Bridge clearly do not obey the general trend. The number of clusters within ∼ 2° of the SMC centre appears to have increased substantially after ∼2.5 Gyr ago, hinting at a burst.
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: Geisler, Doug. Universidad de Concepción; Chile
Fil: Sarajedini, Ata. University of Florida; Estados Unidos
Fil: Gallart, Carme. Instituto de Astrof´ısica de Canarias; España
Fil: Wischnjewsky, Marina. Universidad de Chile; Chile
Materia
CLUSTER
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:11336/21039
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Seven young star clusters in the inner region of the Small Magellanic CloudPiatti, Andres EduardoGeisler, DougSarajedini, AtaGallart, CarmeWischnjewsky, MarinaCLUSTERhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present CCD photometry in the Washington system C and T1 passbands down to T1∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T1 magnitudes and C−T1 colours for a total of 114 826 stars distributed throughout cluster areas of 13.7 × 13.7 arcmin2 each. Cluster radii were estimated from star counts distributed throughout the entire observed fields. The seven clusters are generally characterized by a relatively small angular size and by a high field star contamination. We performed an in-depth analysis of the field star contamination of the colour–magnitude diagrams (CMDs), and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T1, C−T1) CMDs, we derive ages for the sample, assuming Z= 0.004, finding ages between 25 Myr and 1.2 Gyr. We then examined different relationships between positions in the SMC, age and metallicity of a larger sample of clusters including our previous work whose ages and metallicities are on the same scale used in this paper. We confirm previous results in the sense that the further a cluster is from the centre of the galaxy, the older and more metal poor it is, with some dispersion; although clusters associated with the Magellanic Bridge clearly do not obey the general trend. The number of clusters within ∼ 2° of the SMC centre appears to have increased substantially after ∼2.5 Gyr ago, hinting at a burst.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; ArgentinaFil: Geisler, Doug. Universidad de Concepción; ChileFil: Sarajedini, Ata. University of Florida; Estados UnidosFil: Gallart, Carme. Instituto de Astrof´ısica de Canarias; EspañaFil: Wischnjewsky, Marina. Universidad de Chile; ChileWiley Blackwell Publishing, Inc2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21039Piatti, Andres Eduardo; Geisler, Doug; Sarajedini, Ata; Gallart, Carme; Wischnjewsky, Marina; Seven young star clusters in the inner region of the Small Magellanic Cloud; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 389; 1; 12-2008; 429-4400035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.13593.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2008.13593.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 Técnicas2025-09-29T10:18:37Zoai:ri.conicet.gov.ar:11336/21039instacron: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 10:18:37.338CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Seven young star clusters in the inner region of the Small Magellanic Cloud
title Seven young star clusters in the inner region of the Small Magellanic Cloud
spellingShingle Seven young star clusters in the inner region of the Small Magellanic Cloud
Piatti, Andres Eduardo
CLUSTER
title_short Seven young star clusters in the inner region of the Small Magellanic Cloud
title_full Seven young star clusters in the inner region of the Small Magellanic Cloud
title_fullStr Seven young star clusters in the inner region of the Small Magellanic Cloud
title_full_unstemmed Seven young star clusters in the inner region of the Small Magellanic Cloud
title_sort Seven young star clusters in the inner region of the Small Magellanic Cloud
dc.creator.none.fl_str_mv Piatti, Andres Eduardo
Geisler, Doug
Sarajedini, Ata
Gallart, Carme
Wischnjewsky, Marina
author Piatti, Andres Eduardo
author_facet Piatti, Andres Eduardo
Geisler, Doug
Sarajedini, Ata
Gallart, Carme
Wischnjewsky, Marina
author_role author
author2 Geisler, Doug
Sarajedini, Ata
Gallart, Carme
Wischnjewsky, Marina
author2_role author
author
author
author
dc.subject.none.fl_str_mv CLUSTER
topic CLUSTER
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 CCD photometry in the Washington system C and T1 passbands down to T1∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T1 magnitudes and C−T1 colours for a total of 114 826 stars distributed throughout cluster areas of 13.7 × 13.7 arcmin2 each. Cluster radii were estimated from star counts distributed throughout the entire observed fields. The seven clusters are generally characterized by a relatively small angular size and by a high field star contamination. We performed an in-depth analysis of the field star contamination of the colour–magnitude diagrams (CMDs), and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T1, C−T1) CMDs, we derive ages for the sample, assuming Z= 0.004, finding ages between 25 Myr and 1.2 Gyr. We then examined different relationships between positions in the SMC, age and metallicity of a larger sample of clusters including our previous work whose ages and metallicities are on the same scale used in this paper. We confirm previous results in the sense that the further a cluster is from the centre of the galaxy, the older and more metal poor it is, with some dispersion; although clusters associated with the Magellanic Bridge clearly do not obey the general trend. The number of clusters within ∼ 2° of the SMC centre appears to have increased substantially after ∼2.5 Gyr ago, hinting at a burst.
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: Geisler, Doug. Universidad de Concepción; Chile
Fil: Sarajedini, Ata. University of Florida; Estados Unidos
Fil: Gallart, Carme. Instituto de Astrof´ısica de Canarias; España
Fil: Wischnjewsky, Marina. Universidad de Chile; Chile
description We present CCD photometry in the Washington system C and T1 passbands down to T1∼ 22 in the fields of L35, L45, L49, L50, L62, L63 and L85, seven poorly studied star clusters in the inner region of the Small Magellanic Cloud (SMC). We measured T1 magnitudes and C−T1 colours for a total of 114 826 stars distributed throughout cluster areas of 13.7 × 13.7 arcmin2 each. Cluster radii were estimated from star counts distributed throughout the entire observed fields. The seven clusters are generally characterized by a relatively small angular size and by a high field star contamination. We performed an in-depth analysis of the field star contamination of the colour–magnitude diagrams (CMDs), and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T1, C−T1) CMDs, we derive ages for the sample, assuming Z= 0.004, finding ages between 25 Myr and 1.2 Gyr. We then examined different relationships between positions in the SMC, age and metallicity of a larger sample of clusters including our previous work whose ages and metallicities are on the same scale used in this paper. We confirm previous results in the sense that the further a cluster is from the centre of the galaxy, the older and more metal poor it is, with some dispersion; although clusters associated with the Magellanic Bridge clearly do not obey the general trend. The number of clusters within ∼ 2° of the SMC centre appears to have increased substantially after ∼2.5 Gyr ago, hinting at a burst.
publishDate 2008
dc.date.none.fl_str_mv 2008-12
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/11336/21039
Piatti, Andres Eduardo; Geisler, Doug; Sarajedini, Ata; Gallart, Carme; Wischnjewsky, Marina; Seven young star clusters in the inner region of the Small Magellanic Cloud; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 389; 1; 12-2008; 429-440
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21039
identifier_str_mv Piatti, Andres Eduardo; Geisler, Doug; Sarajedini, Ata; Gallart, Carme; Wischnjewsky, Marina; Seven young star clusters in the inner region of the Small Magellanic Cloud; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 389; 1; 12-2008; 429-440
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/doi/10.1111/j.1365-2966.2008.13593.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2008.13593.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
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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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