Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient
Autor(a) principal: | |
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Data de Publicação: | 2018 |
Outros Autores: | , , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/194238 |
Resumo: | We present a semi-empirical, largelymodel-independent approach for estimatingGalactic birth radii, rbirth, for Milky Way disc stars. The technique relies on the justifiable assumption that a negative radial metallicity gradient in the interstellar medium (ISM) existed for most of the disc lifetime. Stars are projected back to their birth positions according to the observationally derived age and [Fe/H] with no kinematical information required. Applying our approach to the AMBRE:HARPS and HARPS–GTO local samples, we show that we can constrain the ISM metallicity evolution with Galactic radius and cosmic time, [Fe/H]ISM(r, t), by requiring a physically meaningful rbirth distribution. We find that the data are consistent with an ISM radial metallicity gradient that flattens with time from ~− 0.15 dex kpc−1 at the beginning of disc formation, to its measured present-day value (−0.07 dex kpc−1). We present several chemokinematical relations in terms of mono-rbirth populations. One remarkable result is that the kinematically hottest stars would have been born locally or in the outer disc, consistent with thick disc formation from the nested flares of mono-age populations and predictions from cosmological simulations. This phenomenon can be also seen in the observed age–velocity dispersion relation, in that its upper boundary is dominated by stars born at larger radii. We also find that the flatness of the local age–metallicity relation (AMR) is the result of the superposition of the AMRs of mono-rbirth populations, each with a well-defined negative slope. The solar birth radius is estimated to be 7.3 ± 0.6 kpc, for a current Galactocentric radius of 8 kpc. |
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Minchev, IvanAnders, FriedrichRecio-Blanco, AlejandraChiappini, C.C.M.Laverny, Patrick deQueiroz, Anna Bárbara de AndradeSteinmetz, M.Adibekyan, VardanCarrillo, IsmaelCescutti, GabrieleGuiglion, GuillaumeHayden, MichaelJong, Roelof S. deKordopatis, GeorgesMajewski, Steven RaymondMartig, MarieSantiago, Basilio Xavier2019-05-15T02:37:50Z20180035-8711http://hdl.handle.net/10183/194238001086167We present a semi-empirical, largelymodel-independent approach for estimatingGalactic birth radii, rbirth, for Milky Way disc stars. The technique relies on the justifiable assumption that a negative radial metallicity gradient in the interstellar medium (ISM) existed for most of the disc lifetime. Stars are projected back to their birth positions according to the observationally derived age and [Fe/H] with no kinematical information required. Applying our approach to the AMBRE:HARPS and HARPS–GTO local samples, we show that we can constrain the ISM metallicity evolution with Galactic radius and cosmic time, [Fe/H]ISM(r, t), by requiring a physically meaningful rbirth distribution. We find that the data are consistent with an ISM radial metallicity gradient that flattens with time from ~− 0.15 dex kpc−1 at the beginning of disc formation, to its measured present-day value (−0.07 dex kpc−1). We present several chemokinematical relations in terms of mono-rbirth populations. One remarkable result is that the kinematically hottest stars would have been born locally or in the outer disc, consistent with thick disc formation from the nested flares of mono-age populations and predictions from cosmological simulations. This phenomenon can be also seen in the observed age–velocity dispersion relation, in that its upper boundary is dominated by stars born at larger radii. We also find that the flatness of the local age–metallicity relation (AMR) is the result of the superposition of the AMRs of mono-rbirth populations, each with a well-defined negative slope. The solar birth radius is estimated to be 7.3 ± 0.6 kpc, for a current Galactocentric radius of 8 kpc.application/pdfengMonthly notices of the royal astronomical society. Oxford. Vol. 481, no. 2 (Dec. 2018), p. 1645-1657Evolucao galaticaFormacao de galaxiasCinemáticaMetalicidadeMeio interestelarISM: abundancesGalaxy: abundancesGalaxy: discGalaxy: evolutionGalaxy: formationGalaxy: kinematics and dynamicsGalaxy: solar neighbourhoodGalaxies: ISMEstimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradientEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSTEXT001086167.pdf.txt001086167.pdf.txtExtracted Texttext/plain70029http://www.lume.ufrgs.br/bitstream/10183/194238/2/001086167.pdf.txt69a67408b068108521583fd5fe92db56MD52ORIGINAL001086167.pdfTexto completo (inglês)application/pdf930365http://www.lume.ufrgs.br/bitstream/10183/194238/1/001086167.pdf08acad4f6b061734a82a6b70aea0a7daMD5110183/1942382023-07-02 03:41:16.70714oai:www.lume.ufrgs.br:10183/194238Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-02T06:41:16Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
title |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
spellingShingle |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient Minchev, Ivan Evolucao galatica Formacao de galaxias Cinemática Metalicidade Meio interestelar ISM: abundances Galaxy: abundances Galaxy: disc Galaxy: evolution Galaxy: formation Galaxy: kinematics and dynamics Galaxy: solar neighbourhood Galaxies: ISM |
title_short |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
title_full |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
title_fullStr |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
title_full_unstemmed |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
title_sort |
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient |
author |
Minchev, Ivan |
author_facet |
Minchev, Ivan Anders, Friedrich Recio-Blanco, Alejandra Chiappini, C.C.M. Laverny, Patrick de Queiroz, Anna Bárbara de Andrade Steinmetz, M. Adibekyan, Vardan Carrillo, Ismael Cescutti, Gabriele Guiglion, Guillaume Hayden, Michael Jong, Roelof S. de Kordopatis, Georges Majewski, Steven Raymond Martig, Marie Santiago, Basilio Xavier |
author_role |
author |
author2 |
Anders, Friedrich Recio-Blanco, Alejandra Chiappini, C.C.M. Laverny, Patrick de Queiroz, Anna Bárbara de Andrade Steinmetz, M. Adibekyan, Vardan Carrillo, Ismael Cescutti, Gabriele Guiglion, Guillaume Hayden, Michael Jong, Roelof S. de Kordopatis, Georges Majewski, Steven Raymond Martig, Marie Santiago, Basilio Xavier |
author2_role |
author author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Minchev, Ivan Anders, Friedrich Recio-Blanco, Alejandra Chiappini, C.C.M. Laverny, Patrick de Queiroz, Anna Bárbara de Andrade Steinmetz, M. Adibekyan, Vardan Carrillo, Ismael Cescutti, Gabriele Guiglion, Guillaume Hayden, Michael Jong, Roelof S. de Kordopatis, Georges Majewski, Steven Raymond Martig, Marie Santiago, Basilio Xavier |
dc.subject.por.fl_str_mv |
Evolucao galatica Formacao de galaxias Cinemática Metalicidade Meio interestelar |
topic |
Evolucao galatica Formacao de galaxias Cinemática Metalicidade Meio interestelar ISM: abundances Galaxy: abundances Galaxy: disc Galaxy: evolution Galaxy: formation Galaxy: kinematics and dynamics Galaxy: solar neighbourhood Galaxies: ISM |
dc.subject.eng.fl_str_mv |
ISM: abundances Galaxy: abundances Galaxy: disc Galaxy: evolution Galaxy: formation Galaxy: kinematics and dynamics Galaxy: solar neighbourhood Galaxies: ISM |
description |
We present a semi-empirical, largelymodel-independent approach for estimatingGalactic birth radii, rbirth, for Milky Way disc stars. The technique relies on the justifiable assumption that a negative radial metallicity gradient in the interstellar medium (ISM) existed for most of the disc lifetime. Stars are projected back to their birth positions according to the observationally derived age and [Fe/H] with no kinematical information required. Applying our approach to the AMBRE:HARPS and HARPS–GTO local samples, we show that we can constrain the ISM metallicity evolution with Galactic radius and cosmic time, [Fe/H]ISM(r, t), by requiring a physically meaningful rbirth distribution. We find that the data are consistent with an ISM radial metallicity gradient that flattens with time from ~− 0.15 dex kpc−1 at the beginning of disc formation, to its measured present-day value (−0.07 dex kpc−1). We present several chemokinematical relations in terms of mono-rbirth populations. One remarkable result is that the kinematically hottest stars would have been born locally or in the outer disc, consistent with thick disc formation from the nested flares of mono-age populations and predictions from cosmological simulations. This phenomenon can be also seen in the observed age–velocity dispersion relation, in that its upper boundary is dominated by stars born at larger radii. We also find that the flatness of the local age–metallicity relation (AMR) is the result of the superposition of the AMRs of mono-rbirth populations, each with a well-defined negative slope. The solar birth radius is estimated to be 7.3 ± 0.6 kpc, for a current Galactocentric radius of 8 kpc. |
publishDate |
2018 |
dc.date.issued.fl_str_mv |
2018 |
dc.date.accessioned.fl_str_mv |
2019-05-15T02:37:50Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/194238 |
dc.identifier.issn.pt_BR.fl_str_mv |
0035-8711 |
dc.identifier.nrb.pt_BR.fl_str_mv |
001086167 |
identifier_str_mv |
0035-8711 001086167 |
url |
http://hdl.handle.net/10183/194238 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Monthly notices of the royal astronomical society. Oxford. Vol. 481, no. 2 (Dec. 2018), p. 1645-1657 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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application/pdf |
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