The star field age-metallicity relationship of the Small Magellanic Cloud
- Autores
- Piatti, Andres Eduardo
- Año de publicación
- 2012
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present the results of the age and metallicity estimates for the unprecedented data base of some 3.3 million stars distributed throughout the entire Small Magellanic Cloud main body, obtained for the first time from CCD Washington CT1 photometry. We produce the first comprehensive star field age–metallicity relationship (AMR) from the birth of the galaxy until ∼1 Gyr ago, independent of any other previous approach. We find that the field stars do not possess gradients in age and metallicity, and that stellar populations formed since ∼2 Gyr ago are more metal rich than [Fe/H] ∼−0.8 dex and are confined to the innermost region (semi-major axis ≲ 1°). For the first time, we compare, homogeneously, the present star field AMR to that of the star cluster population with ages and metallicities in the same star field scales, and find that clusters and star fields share similar chemical evolution histories. Both galaxy components have experienced two enhanced formation processes: the most recent peaked at an age of ∼2 Gyr, and an earlier one detected at an age of ∼5–6 and 7.5 Gyr for clusters and star fields, respectively.
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 - Materia
- cluster
- 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:11336/18623
Ver los metadatos del registro completo
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The star field age-metallicity relationship of the Small Magellanic CloudPiatti, Andres Eduardoclusterhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present the results of the age and metallicity estimates for the unprecedented data base of some 3.3 million stars distributed throughout the entire Small Magellanic Cloud main body, obtained for the first time from CCD Washington CT1 photometry. We produce the first comprehensive star field age–metallicity relationship (AMR) from the birth of the galaxy until ∼1 Gyr ago, independent of any other previous approach. We find that the field stars do not possess gradients in age and metallicity, and that stellar populations formed since ∼2 Gyr ago are more metal rich than [Fe/H] ∼−0.8 dex and are confined to the innermost region (semi-major axis ≲ 1°). For the first time, we compare, homogeneously, the present star field AMR to that of the star cluster population with ages and metallicities in the same star field scales, and find that clusters and star fields share similar chemical evolution histories. Both galaxy components have experienced two enhanced formation processes: the most recent peaked at an age of ∼2 Gyr, and an earlier one detected at an age of ∼5–6 and 7.5 Gyr for clusters and star fields, respectively.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; ArgentinaOxford University Press2012-03-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/18623Piatti, Andres Eduardo; The star field age-metallicity relationship of the Small Magellanic Cloud; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 422; 2; 2-3-2012; 1109-11210035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2012.20684.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2012.20684.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 Técnicas2025-10-22T11:14:30Zoai:ri.conicet.gov.ar:11336/18623instacron: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 11:14:30.629CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| title |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| spellingShingle |
The star field age-metallicity relationship of the Small Magellanic Cloud Piatti, Andres Eduardo cluster |
| title_short |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| title_full |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| title_fullStr |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| title_full_unstemmed |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| title_sort |
The star field age-metallicity relationship of the Small Magellanic Cloud |
| dc.creator.none.fl_str_mv |
Piatti, Andres Eduardo |
| author |
Piatti, Andres Eduardo |
| author_facet |
Piatti, Andres Eduardo |
| author_role |
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 the results of the age and metallicity estimates for the unprecedented data base of some 3.3 million stars distributed throughout the entire Small Magellanic Cloud main body, obtained for the first time from CCD Washington CT1 photometry. We produce the first comprehensive star field age–metallicity relationship (AMR) from the birth of the galaxy until ∼1 Gyr ago, independent of any other previous approach. We find that the field stars do not possess gradients in age and metallicity, and that stellar populations formed since ∼2 Gyr ago are more metal rich than [Fe/H] ∼−0.8 dex and are confined to the innermost region (semi-major axis ≲ 1°). For the first time, we compare, homogeneously, the present star field AMR to that of the star cluster population with ages and metallicities in the same star field scales, and find that clusters and star fields share similar chemical evolution histories. Both galaxy components have experienced two enhanced formation processes: the most recent peaked at an age of ∼2 Gyr, and an earlier one detected at an age of ∼5–6 and 7.5 Gyr for clusters and star fields, respectively. 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 |
| description |
We present the results of the age and metallicity estimates for the unprecedented data base of some 3.3 million stars distributed throughout the entire Small Magellanic Cloud main body, obtained for the first time from CCD Washington CT1 photometry. We produce the first comprehensive star field age–metallicity relationship (AMR) from the birth of the galaxy until ∼1 Gyr ago, independent of any other previous approach. We find that the field stars do not possess gradients in age and metallicity, and that stellar populations formed since ∼2 Gyr ago are more metal rich than [Fe/H] ∼−0.8 dex and are confined to the innermost region (semi-major axis ≲ 1°). For the first time, we compare, homogeneously, the present star field AMR to that of the star cluster population with ages and metallicities in the same star field scales, and find that clusters and star fields share similar chemical evolution histories. Both galaxy components have experienced two enhanced formation processes: the most recent peaked at an age of ∼2 Gyr, and an earlier one detected at an age of ∼5–6 and 7.5 Gyr for clusters and star fields, respectively. |
| publishDate |
2012 |
| dc.date.none.fl_str_mv |
2012-03-02 |
| 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 |
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publishedVersion |
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http://hdl.handle.net/11336/18623 Piatti, Andres Eduardo; The star field age-metallicity relationship of the Small Magellanic Cloud; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 422; 2; 2-3-2012; 1109-1121 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/18623 |
| identifier_str_mv |
Piatti, Andres Eduardo; The star field age-metallicity relationship of the Small Magellanic Cloud; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 422; 2; 2-3-2012; 1109-1121 0035-8711 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
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eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2012.20684.x info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2012.20684.x |
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Oxford University Press |
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Oxford University Press |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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