Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity

Two main scenarios for the formation of the Galactic bulge are invoked, the first one through gravitational collapse or hierarchical merging of subclumps, the second through secular evolution of the Galactic disc. We aim to constrain the formation of the Galactic bulge through studies of the correla...

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Detalles Bibliográficos
Autores: Babusiaux, C., Zoccali, M., Minniti, D.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2010
País:Chile
Idioma:inglés
OAI Identifier:oai:repositorio.anid.cl:10533/237142
Acceso en línea:https://hdl.handle.net/10533/237142
Access Level:acceso abierto
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spelling Minniti, D.Zoccali, M.Babusiaux, C.201010.1051/0004-6361/201014353https://hdl.handle.net/10533/237142http://purl.org/coar/access_right/c_abf2Insights on the Milky Way bulge formation from the correlations between kinematics and metallicityBabusiaux, C.Zoccali, M.Minniti, D.2019-12-18T18:14:52Z2022-07-07T22:04:58Z2019-12-18T18:14:52Z2022-07-07T22:04:58Z2010Two main scenarios for the formation of the Galactic bulge are invoked, the first one through gravitational collapse or hierarchical merging of subclumps, the second through secular evolution of the Galactic disc. We aim to constrain the formation of the Galactic bulge through studies of the correlation between kinematics and metallicities in Baade's Window (l=1, b=-4) and two other fields along the bulge minor axis (l=0, b=-6 and b=-12). We combine the radial velocity and the [Fe/H] measurements obtained with FLAMES/GIRAFFE at the VLT with a spectral resolution of R=20000, plus for the Baade's Window field the OGLE-II proper motions, and compare these with published N-body simulations of the Galactic bulge. We confirm the presence of two distinct populations in Baade's Window found in Hill et al. 2010: the metal-rich population presents bar-like kinematics while the metal-poor population shows kinematics corresponding to an old spheroid or a thick disc one. In this context the metallicity gradient along the bulge minor axis observed by Zoccali et al. (2008), visible also in the kinematics, can be related to a varying mix of these two populations as one moves away from the Galactic plane, alleviating the apparent contradiction between the kinematic evidence of a bar and the existence of a metallicity gradient. We show evidences that the two main scenarios for the bulge formation co-exist within the Milky Way bulge.FONDAPFONDAP1501000315010003virtual::19444-1WOS:000283297300077https://hdl.handle.net/10533/237142enginstname: Conicytreponame: Repositorio Digital RI2.010.1051/0004-6361/201014353info:eu-repo/grantAgreement/Fondap/15010003https://arxiv.org/abs/1005.3919Atribución-NoComercial-SinDerivadas 3.0 Chilehttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/info:eu-repo/semantics/openAccessInsights on the Milky Way bulge formation from the correlations between kinematics and metallicityAstronomy & AstrophysicsArticuloinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttps://hdl.handle.net/10533/237142http://purl.org/coar/resource_type/c_2df8fbb1045fc0e1-ef55-4532-8afe-69fe789d964dvirtual::19444-1045fc0e1-ef55-4532-8afe-69fe789d964dvirtual::19444-110533/237142oai:repositorio.anid.cl:10533/2371422023-07-24 19:55:17.714https://repositorio.anid.clRepositorio ANIDaletelier@anid.cl
dc.title.none.fl_str_mv Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
dc.title.journal.none.fl_str_mv Astronomy & Astrophysics
title Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
spellingShingle Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
Babusiaux, C.
title_short Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
title_full Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
title_fullStr Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
title_full_unstemmed Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
title_sort Insights on the Milky Way bulge formation from the correlations between kinematics and metallicity
dc.creator.none.fl_str_mv Babusiaux, C.
Zoccali, M.
Minniti, D.
author Babusiaux, C.
author_facet Babusiaux, C.
Zoccali, M.
Minniti, D.
author_role author
author2 Zoccali, M.
Minniti, D.
author2_role author
author
description Two main scenarios for the formation of the Galactic bulge are invoked, the first one through gravitational collapse or hierarchical merging of subclumps, the second through secular evolution of the Galactic disc. We aim to constrain the formation of the Galactic bulge through studies of the correlation between kinematics and metallicities in Baade's Window (l=1, b=-4) and two other fields along the bulge minor axis (l=0, b=-6 and b=-12). We combine the radial velocity and the [Fe/H] measurements obtained with FLAMES/GIRAFFE at the VLT with a spectral resolution of R=20000, plus for the Baade's Window field the OGLE-II proper motions, and compare these with published N-body simulations of the Galactic bulge. We confirm the presence of two distinct populations in Baade's Window found in Hill et al. 2010: the metal-rich population presents bar-like kinematics while the metal-poor population shows kinematics corresponding to an old spheroid or a thick disc one. In this context the metallicity gradient along the bulge minor axis observed by Zoccali et al. (2008), visible also in the kinematics, can be related to a varying mix of these two populations as one moves away from the Galactic plane, alleviating the apparent contradiction between the kinematic evidence of a bar and the existence of a metallicity gradient. We show evidences that the two main scenarios for the bulge formation co-exist within the Milky Way bulge.
publishDate 2010
dc.date.issued.none.fl_str_mv 2010
dc.date.accessioned.none.fl_str_mv 2019-12-18T18:14:52Z
2022-07-07T22:04:58Z
dc.date.available.none.fl_str_mv 2019-12-18T18:14:52Z
2022-07-07T22:04:58Z
dc.type.none.fl_str_mv Articulo
dc.type.driver.none.fl_str_mv info:eu-repo/semantics/article
dc.type.openaire.none.fl_str_mv info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.folio.none.fl_str_mv 15010003
15010003
dc.identifier.idwos.none.fl_str_mv WOS:000283297300077
dc.identifier.uri.none.fl_str_mv https://hdl.handle.net/10533/237142
identifier_str_mv 15010003
WOS:000283297300077
url https://hdl.handle.net/10533/237142
dc.language.iso.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv instname: Conicyt
reponame: Repositorio Digital RI2.0
dc.relation.doi.none.fl_str_mv 10.1051/0004-6361/201014353
dc.relation.projectid.none.fl_str_mv info:eu-repo/grantAgreement/Fondap/15010003
dc.relation.uri.none.fl_str_mv https://arxiv.org/abs/1005.3919
dc.rights.none.fl_str_mv Atribución-NoComercial-SinDerivadas 3.0 Chile
http://creativecommons.org/licenses/by-nc-nd/3.0/cl/
dc.rights.driver.none.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv Atribución-NoComercial-SinDerivadas 3.0 Chile
http://creativecommons.org/licenses/by-nc-nd/3.0/cl/
eu_rights_str_mv openAccess
repository.name.fl_str_mv Repositorio ANID
repository.mail.fl_str_mv aletelier@anid.cl
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score 15,812429

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