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Article: In the thick of it: Metal-poor disc stars in RAVE

TitleIn the thick of it: Metal-poor disc stars in RAVE
Authors
KeywordsGalaxy: kinematics and dynamics
Galaxy: disc
Galaxy: abundances
Galaxy: structure
Galaxy: stellar content
Issue Date2013
Citation
Monthly Notices of the Royal Astronomical Society, 2013, v. 436, n. 4, p. 3231-3246 How to Cite?
AbstractBy selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. We confirm that the metallicity and azimuthal velocity distribution functions of the thick disc are not Gaussian. In particular, we find that the thick disc has an extended metallicity tail going at least down to [M/H] = -2 dex, contributing roughly 3 per cent of the entire thick disc population and having a shorter scalelength compared to the canonical thick disc. The mean azimuthal velocity of these metal-poor stars allows us to estimate the correlation between the metallicity ([M/H]) and the orbital velocity (VΦ), which is an important constraint on the formation mechanisms of the Galactic thick disc. Given our simple approach, we find ∂VΦ/∂[M/H] ≈50 km s-1 dex-1, which is in very good agreement with previous literature values. We complete the study with a brief discussion on the implications of the formation scenarios for the thick disc and suggest that given the above-mentioned characteristics, a thick disc mainly formed by radial migration mechanisms seems unlikely © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/209015
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806

 

DC FieldValueLanguage
dc.contributor.authorKordopatis, Georges-
dc.contributor.authorGilmore, Gerard F.-
dc.contributor.authorWyse, Rosemary F G-
dc.contributor.authorSteinmetz, Matthias-
dc.contributor.authorSiebert, Arnaud-
dc.contributor.authorBienaymé, Olivier-
dc.contributor.authorMcMillan, Paul J.-
dc.contributor.authorMinchev, Ivan-
dc.contributor.authorZwitter, Tomaž-
dc.contributor.authorGibson, Brad K.-
dc.contributor.authorSeabroke, George M.-
dc.contributor.authorGrebel, Eva K.-
dc.contributor.authorBland-Hawthorn, Joss Bland-
dc.contributor.authorBoeche, Corrado-
dc.contributor.authorFreeman, Kenneth C.-
dc.contributor.authorMunari, Ulisse-
dc.contributor.authorNavarro, Julio F.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorReid, Warren A.-
dc.contributor.authorSiviero, Alessandro-
dc.date.accessioned2015-03-23T02:31:10Z-
dc.date.available2015-03-23T02:31:10Z-
dc.date.issued2013-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2013, v. 436, n. 4, p. 3231-3246-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/209015-
dc.description.abstractBy selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. We confirm that the metallicity and azimuthal velocity distribution functions of the thick disc are not Gaussian. In particular, we find that the thick disc has an extended metallicity tail going at least down to [M/H] = -2 dex, contributing roughly 3 per cent of the entire thick disc population and having a shorter scalelength compared to the canonical thick disc. The mean azimuthal velocity of these metal-poor stars allows us to estimate the correlation between the metallicity ([M/H]) and the orbital velocity (VΦ), which is an important constraint on the formation mechanisms of the Galactic thick disc. Given our simple approach, we find ∂VΦ/∂[M/H] ≈50 km s-1 dex-1, which is in very good agreement with previous literature values. We complete the study with a brief discussion on the implications of the formation scenarios for the thick disc and suggest that given the above-mentioned characteristics, a thick disc mainly formed by radial migration mechanisms seems unlikely © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectGalaxy: kinematics and dynamics-
dc.subjectGalaxy: disc-
dc.subjectGalaxy: abundances-
dc.subjectGalaxy: structure-
dc.subjectGalaxy: stellar content-
dc.titleIn the thick of it: Metal-poor disc stars in RAVE-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1093/mnras/stt1804-
dc.identifier.scopuseid_2-s2.0-84889043647-
dc.identifier.volume436-
dc.identifier.issue4-
dc.identifier.spage3231-
dc.identifier.epage3246-
dc.identifier.eissn1365-2966-

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