Mild evolution of the stellar metallicity gradients of disc galaxies

Autores
Tissera, Patricia Beatriz; Machado, Rubens E. G.; Vilchez, Jose M.; Pedrosa, Susana Elizabeth; Sanchez Blazquez, Patricia; Varela, Silvio
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The metallicity gradients of the stellar populations in disc galaxies and their evolution store relevant information on the disc formation history and on those processes which could mix stars a posteriori, such as migration, bars and/or galaxy-galaxy interactions. Aims. We aim to investigate the evolution of the metallicity gradients of the whole stellar populations in disc components of simulated galaxies in a cosmological context. Methods. We analyse simulated disc galaxies selected from a cosmological hydrodynamical simulation that includes chemical evolution and a physically motivated supernova feedback capable of driving mass-loaded galactic winds. Results. We detect a mild evolution with redshift in the metallicity slopes of − 0.02 ± 0.01 dex kpc-1 from z ~ 1. If the metallicity profiles are normalised by the effective radius of the stellar disc, the slopes show no clear evolution for z< 1, with a median value of approximately − 0.23 dex reff-1. As a function of stellar mass, we find that metallicity gradients steepen for stellar masses smaller than ~1010.3M⊙ while the trend reverses for higher stellar masses, in the redshift range z = [ 0,1 ]. Galaxies with small stellar masses have discs with larger reff and flatter metallicity gradients than expected. We detect migration albeit weaker than in previous works. Conclusions. Our stellar discs show a mild evolution of the stellar metallicity slopes up to z ~ 1, which is well-matched by the evolution calculated archeologically from the abundance distributions of mono-age stellar populations at z ~ 0. The dispersion in the relations allows for stronger individual evolutions. Overall, supernova feedback could explain the trends but an impact of migration can not be totally discarded. Galaxy-galaxy interactions or small satellite accretions can also contribute to modify the metallicity profiles in the outer parts. Disentangling the effects of these processes for individual galaxies is still a challenge in a cosmological context.
Fil: Tissera, Patricia Beatriz. Universidad Andres Bello; Chile. 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: Machado, Rubens E. G.. Universidad Tecnologica Federal de Parana; Brasil. Universidad Andres Bello; Chile. Universidade Federal de Ouro Preto; Brasil
Fil: Vilchez, Jose M.. Instituto de Astrofisica de Andalucia; España
Fil: Pedrosa, Susana Elizabeth. 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: Sanchez Blazquez, Patricia. Universidad Autonoma de Barcelona. Facultad de Física; España
Fil: Varela, Silvio. Universidad Andres Bello; Chile
Materia
galaxy formation
galaxy evolution
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:11336/24181
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/24181
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Mild evolution of the stellar metallicity gradients of disc galaxiesTissera, Patricia BeatrizMachado, Rubens E. G.Vilchez, Jose M.Pedrosa, Susana ElizabethSanchez Blazquez, PatriciaVarela, Silviogalaxy formationgalaxy evolutionhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The metallicity gradients of the stellar populations in disc galaxies and their evolution store relevant information on the disc formation history and on those processes which could mix stars a posteriori, such as migration, bars and/or galaxy-galaxy interactions. Aims. We aim to investigate the evolution of the metallicity gradients of the whole stellar populations in disc components of simulated galaxies in a cosmological context. Methods. We analyse simulated disc galaxies selected from a cosmological hydrodynamical simulation that includes chemical evolution and a physically motivated supernova feedback capable of driving mass-loaded galactic winds. Results. We detect a mild evolution with redshift in the metallicity slopes of − 0.02 ± 0.01 dex kpc-1 from z ~ 1. If the metallicity profiles are normalised by the effective radius of the stellar disc, the slopes show no clear evolution for z< 1, with a median value of approximately − 0.23 dex reff-1. As a function of stellar mass, we find that metallicity gradients steepen for stellar masses smaller than ~1010.3M⊙ while the trend reverses for higher stellar masses, in the redshift range z = [ 0,1 ]. Galaxies with small stellar masses have discs with larger reff and flatter metallicity gradients than expected. We detect migration albeit weaker than in previous works. Conclusions. Our stellar discs show a mild evolution of the stellar metallicity slopes up to z ~ 1, which is well-matched by the evolution calculated archeologically from the abundance distributions of mono-age stellar populations at z ~ 0. The dispersion in the relations allows for stronger individual evolutions. Overall, supernova feedback could explain the trends but an impact of migration can not be totally discarded. Galaxy-galaxy interactions or small satellite accretions can also contribute to modify the metallicity profiles in the outer parts. Disentangling the effects of these processes for individual galaxies is still a challenge in a cosmological context.Fil: Tissera, Patricia Beatriz. Universidad Andres Bello; Chile. 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: Machado, Rubens E. G.. Universidad Tecnologica Federal de Parana; Brasil. Universidad Andres Bello; Chile. Universidade Federal de Ouro Preto; BrasilFil: Vilchez, Jose M.. Instituto de Astrofisica de Andalucia; EspañaFil: Pedrosa, Susana Elizabeth. 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: Sanchez Blazquez, Patricia. Universidad Autonoma de Barcelona. Facultad de Física; EspañaFil: Varela, Silvio. Universidad Andres Bello; ChileEDP Sciences2017-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/24181Tissera, Patricia Beatriz; Machado, Rubens E. G.; Vilchez, Jose M.; Pedrosa, Susana Elizabeth; Sanchez Blazquez, Patricia; et al.; Mild evolution of the stellar metallicity gradients of disc galaxies; EDP Sciences; Astronomy and Astrophysics; 604; A118; 8-2017; 1-80004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628915info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/08/aa28915-16/aa28915-16.htmlinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1706.03739info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:25:21Zoai:ri.conicet.gov.ar:11336/24181instacron: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 10:25:21.86CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Mild evolution of the stellar metallicity gradients of disc galaxies
title Mild evolution of the stellar metallicity gradients of disc galaxies
spellingShingle Mild evolution of the stellar metallicity gradients of disc galaxies
Tissera, Patricia Beatriz
galaxy formation
galaxy evolution
title_short Mild evolution of the stellar metallicity gradients of disc galaxies
title_full Mild evolution of the stellar metallicity gradients of disc galaxies
title_fullStr Mild evolution of the stellar metallicity gradients of disc galaxies
title_full_unstemmed Mild evolution of the stellar metallicity gradients of disc galaxies
title_sort Mild evolution of the stellar metallicity gradients of disc galaxies
dc.creator.none.fl_str_mv Tissera, Patricia Beatriz
Machado, Rubens E. G.
Vilchez, Jose M.
Pedrosa, Susana Elizabeth
Sanchez Blazquez, Patricia
Varela, Silvio
author Tissera, Patricia Beatriz
author_facet Tissera, Patricia Beatriz
Machado, Rubens E. G.
Vilchez, Jose M.
Pedrosa, Susana Elizabeth
Sanchez Blazquez, Patricia
Varela, Silvio
author_role author
author2 Machado, Rubens E. G.
Vilchez, Jose M.
Pedrosa, Susana Elizabeth
Sanchez Blazquez, Patricia
Varela, Silvio
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv galaxy formation
galaxy evolution
topic galaxy formation
galaxy evolution
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. The metallicity gradients of the stellar populations in disc galaxies and their evolution store relevant information on the disc formation history and on those processes which could mix stars a posteriori, such as migration, bars and/or galaxy-galaxy interactions. Aims. We aim to investigate the evolution of the metallicity gradients of the whole stellar populations in disc components of simulated galaxies in a cosmological context. Methods. We analyse simulated disc galaxies selected from a cosmological hydrodynamical simulation that includes chemical evolution and a physically motivated supernova feedback capable of driving mass-loaded galactic winds. Results. We detect a mild evolution with redshift in the metallicity slopes of − 0.02 ± 0.01 dex kpc-1 from z ~ 1. If the metallicity profiles are normalised by the effective radius of the stellar disc, the slopes show no clear evolution for z< 1, with a median value of approximately − 0.23 dex reff-1. As a function of stellar mass, we find that metallicity gradients steepen for stellar masses smaller than ~1010.3M⊙ while the trend reverses for higher stellar masses, in the redshift range z = [ 0,1 ]. Galaxies with small stellar masses have discs with larger reff and flatter metallicity gradients than expected. We detect migration albeit weaker than in previous works. Conclusions. Our stellar discs show a mild evolution of the stellar metallicity slopes up to z ~ 1, which is well-matched by the evolution calculated archeologically from the abundance distributions of mono-age stellar populations at z ~ 0. The dispersion in the relations allows for stronger individual evolutions. Overall, supernova feedback could explain the trends but an impact of migration can not be totally discarded. Galaxy-galaxy interactions or small satellite accretions can also contribute to modify the metallicity profiles in the outer parts. Disentangling the effects of these processes for individual galaxies is still a challenge in a cosmological context.
Fil: Tissera, Patricia Beatriz. Universidad Andres Bello; Chile. 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: Machado, Rubens E. G.. Universidad Tecnologica Federal de Parana; Brasil. Universidad Andres Bello; Chile. Universidade Federal de Ouro Preto; Brasil
Fil: Vilchez, Jose M.. Instituto de Astrofisica de Andalucia; España
Fil: Pedrosa, Susana Elizabeth. 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: Sanchez Blazquez, Patricia. Universidad Autonoma de Barcelona. Facultad de Física; España
Fil: Varela, Silvio. Universidad Andres Bello; Chile
description Context. The metallicity gradients of the stellar populations in disc galaxies and their evolution store relevant information on the disc formation history and on those processes which could mix stars a posteriori, such as migration, bars and/or galaxy-galaxy interactions. Aims. We aim to investigate the evolution of the metallicity gradients of the whole stellar populations in disc components of simulated galaxies in a cosmological context. Methods. We analyse simulated disc galaxies selected from a cosmological hydrodynamical simulation that includes chemical evolution and a physically motivated supernova feedback capable of driving mass-loaded galactic winds. Results. We detect a mild evolution with redshift in the metallicity slopes of − 0.02 ± 0.01 dex kpc-1 from z ~ 1. If the metallicity profiles are normalised by the effective radius of the stellar disc, the slopes show no clear evolution for z< 1, with a median value of approximately − 0.23 dex reff-1. As a function of stellar mass, we find that metallicity gradients steepen for stellar masses smaller than ~1010.3M⊙ while the trend reverses for higher stellar masses, in the redshift range z = [ 0,1 ]. Galaxies with small stellar masses have discs with larger reff and flatter metallicity gradients than expected. We detect migration albeit weaker than in previous works. Conclusions. Our stellar discs show a mild evolution of the stellar metallicity slopes up to z ~ 1, which is well-matched by the evolution calculated archeologically from the abundance distributions of mono-age stellar populations at z ~ 0. The dispersion in the relations allows for stronger individual evolutions. Overall, supernova feedback could explain the trends but an impact of migration can not be totally discarded. Galaxy-galaxy interactions or small satellite accretions can also contribute to modify the metallicity profiles in the outer parts. Disentangling the effects of these processes for individual galaxies is still a challenge in a cosmological context.
publishDate 2017
dc.date.none.fl_str_mv 2017-08
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/11336/24181
Tissera, Patricia Beatriz; Machado, Rubens E. G.; Vilchez, Jose M.; Pedrosa, Susana Elizabeth; Sanchez Blazquez, Patricia; et al.; Mild evolution of the stellar metallicity gradients of disc galaxies; EDP Sciences; Astronomy and Astrophysics; 604; A118; 8-2017; 1-8
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/24181
identifier_str_mv Tissera, Patricia Beatriz; Machado, Rubens E. G.; Vilchez, Jose M.; Pedrosa, Susana Elizabeth; Sanchez Blazquez, Patricia; et al.; Mild evolution of the stellar metallicity gradients of disc galaxies; EDP Sciences; Astronomy and Astrophysics; 604; A118; 8-2017; 1-8
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628915
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/08/aa28915-16/aa28915-16.html
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1706.03739
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 EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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