The star field age-metallicity relationship of the Small Magellanic Cloud

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 CT 1 photometry. We produce the first comprehensive star field age...

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Detalles Bibliográficos
Publicado:	2012
Materias:	Galaxies: individual: Small Magellanic Cloud Galaxies: star clusters: general Magellanic Clouds Techniques: photometric
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v422_n2_p1109_Piatti http://hdl.handle.net/20.500.12110/paper_00358711_v422_n2_p1109_Piatti
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00358711_v422_n2_p1109_Piatti
record_format	dspace
spelling	paper:paper_00358711_v422_n2_p1109_Piatti2023-06-08T15:01:33Z The star field age-metallicity relationship of the Small Magellanic Cloud Galaxies: individual: Small Magellanic Cloud Galaxies: star clusters: general Magellanic Clouds Techniques: photometric 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 CT 1 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. © 2012 The Author Monthly Notices of the Royal Astronomical Society © 2012 RAS. 2012 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v422_n2_p1109_Piatti http://hdl.handle.net/20.500.12110/paper_00358711_v422_n2_p1109_Piatti
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Galaxies: individual: Small Magellanic Cloud Galaxies: star clusters: general Magellanic Clouds Techniques: photometric
spellingShingle	Galaxies: individual: Small Magellanic Cloud Galaxies: star clusters: general Magellanic Clouds Techniques: photometric The star field age-metallicity relationship of the Small Magellanic Cloud
topic_facet	Galaxies: individual: Small Magellanic Cloud Galaxies: star clusters: general Magellanic Clouds Techniques: photometric
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 CT 1 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. © 2012 The Author Monthly Notices of the Royal Astronomical Society © 2012 RAS.
title	The star field age-metallicity relationship of the Small Magellanic Cloud
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	star field age-metallicity relationship of the small magellanic cloud
publishDate	2012
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v422_n2_p1109_Piatti http://hdl.handle.net/20.500.12110/paper_00358711_v422_n2_p1109_Piatti
_version_	1768541598937776128

The star field age-metallicity relationship of the Small Magellanic Cloud

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