Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies

Autores
Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; Martig, Marie
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history.
Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones 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. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Scannapieco, Cecilia. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Houssay; Argentina
Fil: Chiappini, Cristina. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Junqueira, Thiago C.. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Minchev, Ivan. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Martig, Marie. Liverpool John Moores University; Reino Unido
Materia
GALAXIES: EVOLUTION
GALAXIES: FORMATION
HYDRODYNAMICS
INTERGALACTIC MEDIUM
METHODS: NUMERICAL
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:11336/113150

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network_name_str CONICET Digital (CONICET)
spelling Gas accretion in Milky Way-like galaxies: Temporal and radial dependenciesNuza, Sebastian ErnestoScannapieco, CeciliaChiappini, CristinaJunqueira, Thiago C.Minchev, IvanMartig, MarieGALAXIES: EVOLUTIONGALAXIES: FORMATIONHYDRODYNAMICSINTERGALACTIC MEDIUMMETHODS: NUMERICALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history.Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones 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. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Scannapieco, Cecilia. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Houssay; ArgentinaFil: Chiappini, Cristina. Leibniz Institut Fuer Astrophysik Potsdam; AlemaniaFil: Junqueira, Thiago C.. Leibniz Institut Fuer Astrophysik Potsdam; AlemaniaFil: Minchev, Ivan. Leibniz Institut Fuer Astrophysik Potsdam; AlemaniaFil: Martig, Marie. Liverpool John Moores University; Reino UnidoWiley Blackwell Publishing, Inc2019-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/113150Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; et al.; Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 482; 3; 1-2019; 3089-31080035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty2882info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/482/3/3089/5144234info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:51:47Zoai:ri.conicet.gov.ar:11336/113150instacron: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 09:51:48.122CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
title Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
spellingShingle Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
Nuza, Sebastian Ernesto
GALAXIES: EVOLUTION
GALAXIES: FORMATION
HYDRODYNAMICS
INTERGALACTIC MEDIUM
METHODS: NUMERICAL
title_short Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
title_full Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
title_fullStr Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
title_full_unstemmed Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
title_sort Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
dc.creator.none.fl_str_mv Nuza, Sebastian Ernesto
Scannapieco, Cecilia
Chiappini, Cristina
Junqueira, Thiago C.
Minchev, Ivan
Martig, Marie
author Nuza, Sebastian Ernesto
author_facet Nuza, Sebastian Ernesto
Scannapieco, Cecilia
Chiappini, Cristina
Junqueira, Thiago C.
Minchev, Ivan
Martig, Marie
author_role author
author2 Scannapieco, Cecilia
Chiappini, Cristina
Junqueira, Thiago C.
Minchev, Ivan
Martig, Marie
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: EVOLUTION
GALAXIES: FORMATION
HYDRODYNAMICS
INTERGALACTIC MEDIUM
METHODS: NUMERICAL
topic GALAXIES: EVOLUTION
GALAXIES: FORMATION
HYDRODYNAMICS
INTERGALACTIC MEDIUM
METHODS: NUMERICAL
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history.
Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones 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. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Scannapieco, Cecilia. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Houssay; Argentina
Fil: Chiappini, Cristina. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Junqueira, Thiago C.. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Minchev, Ivan. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Martig, Marie. Liverpool John Moores University; Reino Unido
description One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history.
publishDate 2019
dc.date.none.fl_str_mv 2019-01
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/11336/113150
Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; et al.; Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 482; 3; 1-2019; 3089-3108
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/113150
identifier_str_mv Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; et al.; Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 482; 3; 1-2019; 3089-3108
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/doi/10.1093/mnras/sty2882
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/482/3/3089/5144234
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)
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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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