The age–metallicity relationship in the Fornax spheroidal dwarf galaxy

Autores
Piatti, Andres Eduardo; del Pino, Andres; Aparicio, Antonio; Hidalgo, Sebastian L
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We produce a comprehensive field star age–metallicity relationship (AMR) from the earliest epoch until ∼1 Gyr ago for three fields in the Fornax dwarf spheroidal galaxy by using VI photometric data obtained with FORS1 at the VLT. We find that the innermost one does not contain dominant very old stars (age > 12 Gyr), whereas the relatively outer field does not account for representative star field populations younger than ∼3 Gyr. When focusing on the most prominent stellar populations, we find that the derived AMRs are engraved by the evidence of an outside-in star formation process. The studied fields show bimodal metallicity distributions peaked at [Fe/H] = (−0.95 ± 0.15) dex and (−1.15 or −1.25 ± 0.05) dex, respectively, but only during the first half of the entire galaxy lifetime. Furthermore, the more metal-rich population appears to be more numerous in the outer fields, while in the innermost Fornax field the contribution of both metallicity populations seems to be similar. We also find that the metallicity spread ∼6 Gyr ago is remarkable large, while the intrinsic metallicity dispersion at ∼1–2 Gyr results smaller than that for the relatively older generations of stars. We interpret these outcomes as a result of a possible merger of two galaxies that would have triggered a star formation bursting process that peaked between ∼6 and 9 Gyr ago, depending on the position of the field in the galaxy.
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina
Fil: del Pino, Andres. Instituto de Astrofısica de Canarias. Tenerife; España
Fil: Aparicio, Antonio. Instituto de Astrofısica de Canarias. Tenerife; España. Universidad de la Laguna; España
Fil: Hidalgo, Sebastian L. Instituto de Astrofısica de Canarias. Tenerife; España
Materia
techniques: photometric
galaxies: dwarf
galaxies: individual: Fornax
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:11336/34086
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/34086
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The age–metallicity relationship in the Fornax spheroidal dwarf galaxyPiatti, Andres Eduardodel Pino, AndresAparicio, AntonioHidalgo, Sebastian Ltechniques: photometricgalaxies: dwarfgalaxies: individual: Fornaxhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We produce a comprehensive field star age–metallicity relationship (AMR) from the earliest epoch until ∼1 Gyr ago for three fields in the Fornax dwarf spheroidal galaxy by using VI photometric data obtained with FORS1 at the VLT. We find that the innermost one does not contain dominant very old stars (age > 12 Gyr), whereas the relatively outer field does not account for representative star field populations younger than ∼3 Gyr. When focusing on the most prominent stellar populations, we find that the derived AMRs are engraved by the evidence of an outside-in star formation process. The studied fields show bimodal metallicity distributions peaked at [Fe/H] = (−0.95 ± 0.15) dex and (−1.15 or −1.25 ± 0.05) dex, respectively, but only during the first half of the entire galaxy lifetime. Furthermore, the more metal-rich population appears to be more numerous in the outer fields, while in the innermost Fornax field the contribution of both metallicity populations seems to be similar. We also find that the metallicity spread ∼6 Gyr ago is remarkable large, while the intrinsic metallicity dispersion at ∼1–2 Gyr results smaller than that for the relatively older generations of stars. We interpret these outcomes as a result of a possible merger of two galaxies that would have triggered a star formation bursting process that peaked between ∼6 and 9 Gyr ago, depending on the position of the field in the galaxy.Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; ArgentinaFil: del Pino, Andres. Instituto de Astrofısica de Canarias. Tenerife; EspañaFil: Aparicio, Antonio. Instituto de Astrofısica de Canarias. Tenerife; España. Universidad de la Laguna; EspañaFil: Hidalgo, Sebastian L. Instituto de Astrofısica de Canarias. Tenerife; EspañaWiley Blackwell Publishing, Inc2014-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/34086Piatti, Andres Eduardo; del Pino, Andres; Aparicio, Antonio; Hidalgo, Sebastian L; The age–metallicity relationship in the Fornax spheroidal dwarf galaxy; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 443; 2; 6-2014; 1748-17530035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/443/2/1748/1069276info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stu1254info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:45:25Zoai:ri.conicet.gov.ar:11336/34086instacron: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:34982025-09-03 09:45:26.007CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
title The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
spellingShingle The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
Piatti, Andres Eduardo
techniques: photometric
galaxies: dwarf
galaxies: individual: Fornax
title_short The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
title_full The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
title_fullStr The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
title_full_unstemmed The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
title_sort The age–metallicity relationship in the Fornax spheroidal dwarf galaxy
dc.creator.none.fl_str_mv Piatti, Andres Eduardo
del Pino, Andres
Aparicio, Antonio
Hidalgo, Sebastian L
author Piatti, Andres Eduardo
author_facet Piatti, Andres Eduardo
del Pino, Andres
Aparicio, Antonio
Hidalgo, Sebastian L
author_role author
author2 del Pino, Andres
Aparicio, Antonio
Hidalgo, Sebastian L
author2_role author
author
author
dc.subject.none.fl_str_mv techniques: photometric
galaxies: dwarf
galaxies: individual: Fornax
topic techniques: photometric
galaxies: dwarf
galaxies: individual: Fornax
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 produce a comprehensive field star age–metallicity relationship (AMR) from the earliest epoch until ∼1 Gyr ago for three fields in the Fornax dwarf spheroidal galaxy by using VI photometric data obtained with FORS1 at the VLT. We find that the innermost one does not contain dominant very old stars (age > 12 Gyr), whereas the relatively outer field does not account for representative star field populations younger than ∼3 Gyr. When focusing on the most prominent stellar populations, we find that the derived AMRs are engraved by the evidence of an outside-in star formation process. The studied fields show bimodal metallicity distributions peaked at [Fe/H] = (−0.95 ± 0.15) dex and (−1.15 or −1.25 ± 0.05) dex, respectively, but only during the first half of the entire galaxy lifetime. Furthermore, the more metal-rich population appears to be more numerous in the outer fields, while in the innermost Fornax field the contribution of both metallicity populations seems to be similar. We also find that the metallicity spread ∼6 Gyr ago is remarkable large, while the intrinsic metallicity dispersion at ∼1–2 Gyr results smaller than that for the relatively older generations of stars. We interpret these outcomes as a result of a possible merger of two galaxies that would have triggered a star formation bursting process that peaked between ∼6 and 9 Gyr ago, depending on the position of the field in the galaxy.
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina
Fil: del Pino, Andres. Instituto de Astrofısica de Canarias. Tenerife; España
Fil: Aparicio, Antonio. Instituto de Astrofısica de Canarias. Tenerife; España. Universidad de la Laguna; España
Fil: Hidalgo, Sebastian L. Instituto de Astrofısica de Canarias. Tenerife; España
description We produce a comprehensive field star age–metallicity relationship (AMR) from the earliest epoch until ∼1 Gyr ago for three fields in the Fornax dwarf spheroidal galaxy by using VI photometric data obtained with FORS1 at the VLT. We find that the innermost one does not contain dominant very old stars (age > 12 Gyr), whereas the relatively outer field does not account for representative star field populations younger than ∼3 Gyr. When focusing on the most prominent stellar populations, we find that the derived AMRs are engraved by the evidence of an outside-in star formation process. The studied fields show bimodal metallicity distributions peaked at [Fe/H] = (−0.95 ± 0.15) dex and (−1.15 or −1.25 ± 0.05) dex, respectively, but only during the first half of the entire galaxy lifetime. Furthermore, the more metal-rich population appears to be more numerous in the outer fields, while in the innermost Fornax field the contribution of both metallicity populations seems to be similar. We also find that the metallicity spread ∼6 Gyr ago is remarkable large, while the intrinsic metallicity dispersion at ∼1–2 Gyr results smaller than that for the relatively older generations of stars. We interpret these outcomes as a result of a possible merger of two galaxies that would have triggered a star formation bursting process that peaked between ∼6 and 9 Gyr ago, depending on the position of the field in the galaxy.
publishDate 2014
dc.date.none.fl_str_mv 2014-06
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/11336/34086
Piatti, Andres Eduardo; del Pino, Andres; Aparicio, Antonio; Hidalgo, Sebastian L; The age–metallicity relationship in the Fornax spheroidal dwarf galaxy; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 443; 2; 6-2014; 1748-1753
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/34086
identifier_str_mv Piatti, Andres Eduardo; del Pino, Andres; Aparicio, Antonio; Hidalgo, Sebastian L; The age–metallicity relationship in the Fornax spheroidal dwarf galaxy; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 443; 2; 6-2014; 1748-1753
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/443/2/1748/1069276
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stu1254
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
_version_ 1842268730786054144
score 13.13397

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