The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE
| Autor(a) principal: | |
|---|---|
| Data de Publicação: | 2019 |
| Outros Autores: | , , , , , , , , , , , , , |
| Tipo de documento: | Artigo |
| Idioma: | eng |
| Título da fonte: | Repositório Institucional da UFRGS |
| Texto Completo: | http://hdl.handle.net/10183/198572 |
Resumo: | We report an analysis of the metal-rich tail ([Fe/H]>−0.75) of stars located at distances fromthe Galactic plane up to|z|∼10 kpc, observed by the Apache Point Observatory GalacticEvolution Experiment (APOGEE). We examine the chemistry, kinematics, and dynamicsof this metal-rich sample using chemical abundances and radial velocities provided by the14th APOGEE data release (DR14) and proper motions from the secondGaiadata release(DR2). The analysis reveals three chemically different stellar populations in the [Mg/Fe]versus[Fe/H]space–ahigh-[Mg/Fe]andlow-[Mg/Fe]populations, and a third group withintermediate [Mg/Fe]∼+0.1 – as well as for other chemical elements. We find that they arealso kinematically and dynamically distinct. The high-[Mg/Fe] population exhibits a prograderotation which decreases down to 0 as|zmax|increases, as well as eccentric orbits that aremore bound and closer to the plane. The low-[Mg/Fe] stars are likely Sagittarius members,moving in less-bound orbits reaching larger distances from the centre and the Galactic plane.The intermediate-[Mg/Fe] stars resembles the two stellar overdensities lying about|z|∼5 kpcrecently reported in the literature, for which a disc origin has been claimed. We report theidentification of new members of these two disc-heated overdensities |
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Fernández Alvar, EmmaFernández-Trincado, José GregorioMoreno-Díaz, EdmundoSchuster, William J.Carigi, LeticiaRecio-Blanco, AlejandraBeers, Timothy C.Chiappini, C.C.M.Anders, FriedrichSantiago, Basilio XavierQueiroz, Anna Bárbara de AndradePérez Villegas, Maria de Los AngelesZamora, OlgaGarcía-Hernández, D. A.Ortigoza-Urdaneta, Mario2019-08-29T02:35:01Z20190035-8711http://hdl.handle.net/10183/198572001099000We report an analysis of the metal-rich tail ([Fe/H]>−0.75) of stars located at distances fromthe Galactic plane up to|z|∼10 kpc, observed by the Apache Point Observatory GalacticEvolution Experiment (APOGEE). We examine the chemistry, kinematics, and dynamicsof this metal-rich sample using chemical abundances and radial velocities provided by the14th APOGEE data release (DR14) and proper motions from the secondGaiadata release(DR2). The analysis reveals three chemically different stellar populations in the [Mg/Fe]versus[Fe/H]space–ahigh-[Mg/Fe]andlow-[Mg/Fe]populations, and a third group withintermediate [Mg/Fe]∼+0.1 – as well as for other chemical elements. We find that they arealso kinematically and dynamically distinct. The high-[Mg/Fe] population exhibits a prograderotation which decreases down to 0 as|zmax|increases, as well as eccentric orbits that aremore bound and closer to the plane. The low-[Mg/Fe] stars are likely Sagittarius members,moving in less-bound orbits reaching larger distances from the centre and the Galactic plane.The intermediate-[Mg/Fe] stars resembles the two stellar overdensities lying about|z|∼5 kpcrecently reported in the literature, for which a disc origin has been claimed. We report theidentification of new members of these two disc-heated overdensitiesapplication/pdfengMonthly notices of the royal astronomical society. Oxford. Vol. 487, no. 1 (July 2019), p. 1462-1479Galáxias ativasFormacao de galaxiasCinemática estelarEstrelasGalaxy: haloGalaxy: discGalaxy: formationGalaxy: kinematics and dynamicsGalaxy: stellar contentStars: abundancThe metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEEEstrangeiroinfo: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:UFRGSTEXT001099000.pdf.txt001099000.pdf.txtExtracted Texttext/plain81087http://www.lume.ufrgs.br/bitstream/10183/198572/2/001099000.pdf.txt32adb3b2c2fcd77441449dfb52333201MD52ORIGINAL001099000.pdfTexto completo (inglês)application/pdf2557434http://www.lume.ufrgs.br/bitstream/10183/198572/1/001099000.pdfde65597646949c9739c24bbcb7c6bd0dMD5110183/1985722023-07-02 03:41:50.766383oai:www.lume.ufrgs.br:10183/198572Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-02T06:41:50Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
| dc.title.pt_BR.fl_str_mv |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| title |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| spellingShingle |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE Fernández Alvar, Emma Galáxias ativas Formacao de galaxias Cinemática estelar Estrelas Galaxy: halo Galaxy: disc Galaxy: formation Galaxy: kinematics and dynamics Galaxy: stellar content Stars: abundanc |
| title_short |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| title_full |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| title_fullStr |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| title_full_unstemmed |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| title_sort |
The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE |
| author |
Fernández Alvar, Emma |
| author_facet |
Fernández Alvar, Emma Fernández-Trincado, José Gregorio Moreno-Díaz, Edmundo Schuster, William J. Carigi, Leticia Recio-Blanco, Alejandra Beers, Timothy C. Chiappini, C.C.M. Anders, Friedrich Santiago, Basilio Xavier Queiroz, Anna Bárbara de Andrade Pérez Villegas, Maria de Los Angeles Zamora, Olga García-Hernández, D. A. Ortigoza-Urdaneta, Mario |
| author_role |
author |
| author2 |
Fernández-Trincado, José Gregorio Moreno-Díaz, Edmundo Schuster, William J. Carigi, Leticia Recio-Blanco, Alejandra Beers, Timothy C. Chiappini, C.C.M. Anders, Friedrich Santiago, Basilio Xavier Queiroz, Anna Bárbara de Andrade Pérez Villegas, Maria de Los Angeles Zamora, Olga García-Hernández, D. A. Ortigoza-Urdaneta, Mario |
| author2_role |
author author author author author author author author author author author author author author |
| dc.contributor.author.fl_str_mv |
Fernández Alvar, Emma Fernández-Trincado, José Gregorio Moreno-Díaz, Edmundo Schuster, William J. Carigi, Leticia Recio-Blanco, Alejandra Beers, Timothy C. Chiappini, C.C.M. Anders, Friedrich Santiago, Basilio Xavier Queiroz, Anna Bárbara de Andrade Pérez Villegas, Maria de Los Angeles Zamora, Olga García-Hernández, D. A. Ortigoza-Urdaneta, Mario |
| dc.subject.por.fl_str_mv |
Galáxias ativas Formacao de galaxias Cinemática estelar Estrelas |
| topic |
Galáxias ativas Formacao de galaxias Cinemática estelar Estrelas Galaxy: halo Galaxy: disc Galaxy: formation Galaxy: kinematics and dynamics Galaxy: stellar content Stars: abundanc |
| dc.subject.eng.fl_str_mv |
Galaxy: halo Galaxy: disc Galaxy: formation Galaxy: kinematics and dynamics Galaxy: stellar content Stars: abundanc |
| description |
We report an analysis of the metal-rich tail ([Fe/H]>−0.75) of stars located at distances fromthe Galactic plane up to|z|∼10 kpc, observed by the Apache Point Observatory GalacticEvolution Experiment (APOGEE). We examine the chemistry, kinematics, and dynamicsof this metal-rich sample using chemical abundances and radial velocities provided by the14th APOGEE data release (DR14) and proper motions from the secondGaiadata release(DR2). The analysis reveals three chemically different stellar populations in the [Mg/Fe]versus[Fe/H]space–ahigh-[Mg/Fe]andlow-[Mg/Fe]populations, and a third group withintermediate [Mg/Fe]∼+0.1 – as well as for other chemical elements. We find that they arealso kinematically and dynamically distinct. The high-[Mg/Fe] population exhibits a prograderotation which decreases down to 0 as|zmax|increases, as well as eccentric orbits that aremore bound and closer to the plane. The low-[Mg/Fe] stars are likely Sagittarius members,moving in less-bound orbits reaching larger distances from the centre and the Galactic plane.The intermediate-[Mg/Fe] stars resembles the two stellar overdensities lying about|z|∼5 kpcrecently reported in the literature, for which a disc origin has been claimed. We report theidentification of new members of these two disc-heated overdensities |
| publishDate |
2019 |
| dc.date.accessioned.fl_str_mv |
2019-08-29T02:35:01Z |
| dc.date.issued.fl_str_mv |
2019 |
| dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
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info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
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http://hdl.handle.net/10183/198572 |
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0035-8711 |
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001099000 |
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0035-8711 001099000 |
| url |
http://hdl.handle.net/10183/198572 |
| 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. 487, no. 1 (July 2019), p. 1462-1479 |
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info:eu-repo/semantics/openAccess |
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openAccess |
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