Cardinal kinematics – I. : rotation fields of the APOGEE survey
Autor(a) principal: | |
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Data de Publicação: | 2017 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/159674 |
Resumo: | Correlations between stellar chemistry and kinematics have long been used to gain insight into the evolution of the Milky Way Galaxy. Orbital angular momentum is a key physical parameter and it is often estimated from three-dimensional space motions.We here demonstrate the lower uncertainties that can be achieved in the estimation of one component of velocity through selection of stars in key directions and use of line-of-sight velocity alone (i.e. without incorporation of proper motion data). In this first paper, we apply our technique to stars observed in the direction of Galactic rotation in the APOGEE (Apache Point Observatory Galactic Evolution Experiment) survey.We first derive the distribution of azimuthal velocities, vφ, then from these and observed radial coordinates, estimate the stellar guiding centre radii, Rg, within 6.9 ≤ R ≤ 10 kpc with uncertainties smaller than (or of the order of) 1 kpc. We show that there is no simple way to select a clean stellar sample based on low errors on proper motions and distances to obtain high-quality 3D velocities and hence one should pay particular attention when trying to identify kinematically peculiar stars based on velocities derived using the proper motions. Using our vφ estimations, we investigate the joint distribution of elemental abundances and rotational kinematics free from the blurring effects of epicyclic motions, and we derive the ∂vφ/∂[α/Fe] and ∂vφ/∂[Fe/H] trends for the thin and thick discs as a function of radius. Our analysis provides further evidence for radial migration within the thin disc and hints against radial migration playing a significant role in the evolution of the thick disc. |
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Kordopatis, GeorgesWyse, Rosemary F.G.Chiappini, C.C.M.Minchev, IvanAnders, FriedrichSantiago, Basilio Xavier2017-06-20T02:30:27Z20170035-8711http://hdl.handle.net/10183/159674001022273Correlations between stellar chemistry and kinematics have long been used to gain insight into the evolution of the Milky Way Galaxy. Orbital angular momentum is a key physical parameter and it is often estimated from three-dimensional space motions.We here demonstrate the lower uncertainties that can be achieved in the estimation of one component of velocity through selection of stars in key directions and use of line-of-sight velocity alone (i.e. without incorporation of proper motion data). In this first paper, we apply our technique to stars observed in the direction of Galactic rotation in the APOGEE (Apache Point Observatory Galactic Evolution Experiment) survey.We first derive the distribution of azimuthal velocities, vφ, then from these and observed radial coordinates, estimate the stellar guiding centre radii, Rg, within 6.9 ≤ R ≤ 10 kpc with uncertainties smaller than (or of the order of) 1 kpc. We show that there is no simple way to select a clean stellar sample based on low errors on proper motions and distances to obtain high-quality 3D velocities and hence one should pay particular attention when trying to identify kinematically peculiar stars based on velocities derived using the proper motions. Using our vφ estimations, we investigate the joint distribution of elemental abundances and rotational kinematics free from the blurring effects of epicyclic motions, and we derive the ∂vφ/∂[α/Fe] and ∂vφ/∂[Fe/H] trends for the thin and thick discs as a function of radius. Our analysis provides further evidence for radial migration within the thin disc and hints against radial migration playing a significant role in the evolution of the thick disc.application/pdfengMonthly notices of the Royal Astronomical Society. Oxford. Vol. 467, no. 1 (May 2017), p. 469–489Populacoes estelaresMetalicidadeCinemáticaGalaxy abundancesGalaxy discGalaxy evolutionGalaxy kinematics and dynamicsGalaxy stellar contentCardinal kinematics – I. : rotation fields of the APOGEE surveyEstrangeiroinfo: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:UFRGSORIGINAL001022273.pdf001022273.pdfTexto completo (inglês)application/pdf5674820http://www.lume.ufrgs.br/bitstream/10183/159674/1/001022273.pdf913754efbb0f0050c93d5aebc3a241d4MD51TEXT001022273.pdf.txt001022273.pdf.txtExtracted Texttext/plain89948http://www.lume.ufrgs.br/bitstream/10183/159674/2/001022273.pdf.txt338f3d73c6251574ac4f5a66335d5b15MD5210183/1596742023-07-02 03:41:09.311592oai:www.lume.ufrgs.br:10183/159674Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-02T06:41:09Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
title |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
spellingShingle |
Cardinal kinematics – I. : rotation fields of the APOGEE survey Kordopatis, Georges Populacoes estelares Metalicidade Cinemática Galaxy abundances Galaxy disc Galaxy evolution Galaxy kinematics and dynamics Galaxy stellar content |
title_short |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
title_full |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
title_fullStr |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
title_full_unstemmed |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
title_sort |
Cardinal kinematics – I. : rotation fields of the APOGEE survey |
author |
Kordopatis, Georges |
author_facet |
Kordopatis, Georges Wyse, Rosemary F.G. Chiappini, C.C.M. Minchev, Ivan Anders, Friedrich Santiago, Basilio Xavier |
author_role |
author |
author2 |
Wyse, Rosemary F.G. Chiappini, C.C.M. Minchev, Ivan Anders, Friedrich Santiago, Basilio Xavier |
author2_role |
author author author author author |
dc.contributor.author.fl_str_mv |
Kordopatis, Georges Wyse, Rosemary F.G. Chiappini, C.C.M. Minchev, Ivan Anders, Friedrich Santiago, Basilio Xavier |
dc.subject.por.fl_str_mv |
Populacoes estelares Metalicidade Cinemática |
topic |
Populacoes estelares Metalicidade Cinemática Galaxy abundances Galaxy disc Galaxy evolution Galaxy kinematics and dynamics Galaxy stellar content |
dc.subject.eng.fl_str_mv |
Galaxy abundances Galaxy disc Galaxy evolution Galaxy kinematics and dynamics Galaxy stellar content |
description |
Correlations between stellar chemistry and kinematics have long been used to gain insight into the evolution of the Milky Way Galaxy. Orbital angular momentum is a key physical parameter and it is often estimated from three-dimensional space motions.We here demonstrate the lower uncertainties that can be achieved in the estimation of one component of velocity through selection of stars in key directions and use of line-of-sight velocity alone (i.e. without incorporation of proper motion data). In this first paper, we apply our technique to stars observed in the direction of Galactic rotation in the APOGEE (Apache Point Observatory Galactic Evolution Experiment) survey.We first derive the distribution of azimuthal velocities, vφ, then from these and observed radial coordinates, estimate the stellar guiding centre radii, Rg, within 6.9 ≤ R ≤ 10 kpc with uncertainties smaller than (or of the order of) 1 kpc. We show that there is no simple way to select a clean stellar sample based on low errors on proper motions and distances to obtain high-quality 3D velocities and hence one should pay particular attention when trying to identify kinematically peculiar stars based on velocities derived using the proper motions. Using our vφ estimations, we investigate the joint distribution of elemental abundances and rotational kinematics free from the blurring effects of epicyclic motions, and we derive the ∂vφ/∂[α/Fe] and ∂vφ/∂[Fe/H] trends for the thin and thick discs as a function of radius. Our analysis provides further evidence for radial migration within the thin disc and hints against radial migration playing a significant role in the evolution of the thick disc. |
publishDate |
2017 |
dc.date.accessioned.fl_str_mv |
2017-06-20T02:30:27Z |
dc.date.issued.fl_str_mv |
2017 |
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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publishedVersion |
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http://hdl.handle.net/10183/159674 |
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0035-8711 |
dc.identifier.nrb.pt_BR.fl_str_mv |
001022273 |
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http://hdl.handle.net/10183/159674 |
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. 467, no. 1 (May 2017), p. 469–489 |
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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