Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud
- Autores
- Piatti, Andres Eduardo; Sarajedini, Ata; Geisler, Doug; Clark, David; Seguel, Juan
- Año de publicación
- 2007
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present CCD photometry in the Washington C and T1 filters for six star clusters (B 34, NGC 256, NGC 265, NGC 294, IC 1611 and NGC 376) in the Small Magellanic Cloud (SMC) and their surrounding fields. The resultant colour–magnitude diagrams (CMDs) extend from T1∼ 14 to as faint as T1∼ 22 revealing the main-sequence turnoffs of the clusters. Adopting a metallicity of Z= 0.004, we compare our cluster photometry with theoretical isochrones in the Washington system in order to derive ages. To facilitate age determination of the surrounding fields, we use the magnitude difference between the helium-burning red clump stars and the main-sequence turnoff. Finally, we estimate mean metallicities for the field stars by comparing the location of the field red giant branch with standard giant branches for Galactic globular clusters of known abundance, corrected for age effects. Combining these results with our previous work, we find a clear trend of younger clusters being located closer to the centre of the SMC. In addition, there is a tendency for the mean metallicity and its dispersion to be greater inside 4° of the SMC's centre as compared to outside this radius. As far as the properties of the field stars are concerned, we find little correlation between the ages of the clusters and those of the field stars against which they are projected. Clearly, more work needs to be done to clarify these trends.
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: Sarajedini, Ata. University of Florida; Estados Unidos
Fil: Geisler, Doug. Universidad de Concepción; Chile
Fil: Clark, David. University of Florida; Estados Unidos
Fil: Seguel, Juan. Universidad de Concepción; Chile - 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:11336/21054
Ver los metadatos del registro completo
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Young star clusters immersed in intermediate-age fields in the Small Magellanic CloudPiatti, Andres EduardoSarajedini, AtaGeisler, DougClark, DavidSeguel, Juanhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present CCD photometry in the Washington C and T1 filters for six star clusters (B 34, NGC 256, NGC 265, NGC 294, IC 1611 and NGC 376) in the Small Magellanic Cloud (SMC) and their surrounding fields. The resultant colour–magnitude diagrams (CMDs) extend from T1∼ 14 to as faint as T1∼ 22 revealing the main-sequence turnoffs of the clusters. Adopting a metallicity of Z= 0.004, we compare our cluster photometry with theoretical isochrones in the Washington system in order to derive ages. To facilitate age determination of the surrounding fields, we use the magnitude difference between the helium-burning red clump stars and the main-sequence turnoff. Finally, we estimate mean metallicities for the field stars by comparing the location of the field red giant branch with standard giant branches for Galactic globular clusters of known abundance, corrected for age effects. Combining these results with our previous work, we find a clear trend of younger clusters being located closer to the centre of the SMC. In addition, there is a tendency for the mean metallicity and its dispersion to be greater inside 4° of the SMC's centre as compared to outside this radius. As far as the properties of the field stars are concerned, we find little correlation between the ages of the clusters and those of the field stars against which they are projected. Clearly, more work needs to be done to clarify these trends.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: Sarajedini, Ata. University of Florida; Estados UnidosFil: Geisler, Doug. Universidad de Concepción; ChileFil: Clark, David. University of Florida; Estados UnidosFil: Seguel, Juan. Universidad de Concepción; ChileOxford University Press2007-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21054Piatti, Andres Eduardo; Sarajedini, Ata; Geisler, Doug; Clark, David; Seguel, Juan; Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 377; 1; 12-2007; 300-3160035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2007.11604.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2007.11604.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 Técnicas2025-09-29T10:02:21Zoai:ri.conicet.gov.ar:11336/21054instacron: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 10:02:22.078CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| title |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| spellingShingle |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud Piatti, Andres Eduardo |
| title_short |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| title_full |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| title_fullStr |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| title_full_unstemmed |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| title_sort |
Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud |
| dc.creator.none.fl_str_mv |
Piatti, Andres Eduardo Sarajedini, Ata Geisler, Doug Clark, David Seguel, Juan |
| author |
Piatti, Andres Eduardo |
| author_facet |
Piatti, Andres Eduardo Sarajedini, Ata Geisler, Doug Clark, David Seguel, Juan |
| author_role |
author |
| author2 |
Sarajedini, Ata Geisler, Doug Clark, David Seguel, Juan |
| author2_role |
author author author author |
| 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 C and T1 filters for six star clusters (B 34, NGC 256, NGC 265, NGC 294, IC 1611 and NGC 376) in the Small Magellanic Cloud (SMC) and their surrounding fields. The resultant colour–magnitude diagrams (CMDs) extend from T1∼ 14 to as faint as T1∼ 22 revealing the main-sequence turnoffs of the clusters. Adopting a metallicity of Z= 0.004, we compare our cluster photometry with theoretical isochrones in the Washington system in order to derive ages. To facilitate age determination of the surrounding fields, we use the magnitude difference between the helium-burning red clump stars and the main-sequence turnoff. Finally, we estimate mean metallicities for the field stars by comparing the location of the field red giant branch with standard giant branches for Galactic globular clusters of known abundance, corrected for age effects. Combining these results with our previous work, we find a clear trend of younger clusters being located closer to the centre of the SMC. In addition, there is a tendency for the mean metallicity and its dispersion to be greater inside 4° of the SMC's centre as compared to outside this radius. As far as the properties of the field stars are concerned, we find little correlation between the ages of the clusters and those of the field stars against which they are projected. Clearly, more work needs to be done to clarify these trends. 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: Sarajedini, Ata. University of Florida; Estados Unidos Fil: Geisler, Doug. Universidad de Concepción; Chile Fil: Clark, David. University of Florida; Estados Unidos Fil: Seguel, Juan. Universidad de Concepción; Chile |
| description |
We present CCD photometry in the Washington C and T1 filters for six star clusters (B 34, NGC 256, NGC 265, NGC 294, IC 1611 and NGC 376) in the Small Magellanic Cloud (SMC) and their surrounding fields. The resultant colour–magnitude diagrams (CMDs) extend from T1∼ 14 to as faint as T1∼ 22 revealing the main-sequence turnoffs of the clusters. Adopting a metallicity of Z= 0.004, we compare our cluster photometry with theoretical isochrones in the Washington system in order to derive ages. To facilitate age determination of the surrounding fields, we use the magnitude difference between the helium-burning red clump stars and the main-sequence turnoff. Finally, we estimate mean metallicities for the field stars by comparing the location of the field red giant branch with standard giant branches for Galactic globular clusters of known abundance, corrected for age effects. Combining these results with our previous work, we find a clear trend of younger clusters being located closer to the centre of the SMC. In addition, there is a tendency for the mean metallicity and its dispersion to be greater inside 4° of the SMC's centre as compared to outside this radius. As far as the properties of the field stars are concerned, we find little correlation between the ages of the clusters and those of the field stars against which they are projected. Clearly, more work needs to be done to clarify these trends. |
| publishDate |
2007 |
| dc.date.none.fl_str_mv |
2007-12 |
| 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 |
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article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/21054 Piatti, Andres Eduardo; Sarajedini, Ata; Geisler, Doug; Clark, David; Seguel, Juan; Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 377; 1; 12-2007; 300-316 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/21054 |
| identifier_str_mv |
Piatti, Andres Eduardo; Sarajedini, Ata; Geisler, Doug; Clark, David; Seguel, Juan; Young star clusters immersed in intermediate-age fields in the Small Magellanic Cloud; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 377; 1; 12-2007; 300-316 0035-8711 CONICET Digital CONICET |
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eng |
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eng |
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Oxford University Press |
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Oxford University Press |
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