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Article: Testing formation mechanisms of the Milky Way's thick disc with RAVE

TitleTesting formation mechanisms of the Milky Way's thick disc with RAVE
Authors
KeywordsSolar neighbourhood
Galaxy: disc
Galaxy: formation
Galaxy: structure
Issue Date2011
Citation
Monthly Notices of the Royal Astronomical Society, 2011, v. 413, n. 3, p. 2235-2241 How to Cite?
AbstractWe study the eccentricity distribution of a thick-disc sample of stars (defined as those withVy > 50kms-1and1 < |z|/kpc < 3) observed in the Radial Velocity Experiment (RAVE). We compare this distribution with those obtained in four simulations of galaxy formation taken from the literature as compiled by Sales et al. Each simulation emphasizes different scenarios for the origin of such stars (satellite accretion, heating of a pre-existing thin disc during a merger, radial migration, and gas-rich mergers). We find that the observed distribution peaks at low eccentricities and falls off smoothly and rather steeply to high eccentricities. This finding is fairly robust to changes in distances and to plausible assumptions about thin-disc contamination. Our results favour models where the majority of stars formed in the Galaxy itself on orbits of modest eccentricity and disfavour the pure satellite accretion case. A gas-rich merger origin where most of the stars form 'in situ' appears to be the most consistent with our data. © 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/209002
ISSN
2015 Impact Factor: 4.952
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DC FieldValueLanguage
dc.contributor.authorWilson, Michelle L.-
dc.contributor.authorHelmi, Amina-
dc.contributor.authorMorrison, Heather L.-
dc.contributor.authorBreddels, Maarten A.-
dc.contributor.authorBienaymé, Olivier-
dc.contributor.authorBinney, James J.-
dc.contributor.authorBland-Hawthorn, Joss Bland-
dc.contributor.authorCampbell, Randy D.-
dc.contributor.authorFreeman, Kenneth C.-
dc.contributor.authorFulbright, Jon P.-
dc.contributor.authorGibson, Brad K.-
dc.contributor.authorGilmore, Gerard F.-
dc.contributor.authorGrebel, Eva K.-
dc.contributor.authorMunari, Ulisse-
dc.contributor.authorNavarro, Julio F.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorReid, Warren A.-
dc.contributor.authorSeabroke, George M.-
dc.contributor.authorSiebert, Arnaud-
dc.contributor.authorSiviero, Alessandro-
dc.contributor.authorSteinmetz, Matthias-
dc.contributor.authorWilliams, Mary E K-
dc.contributor.authorWyse, Rosemary F G-
dc.contributor.authorZwitter, Tomaž-
dc.date.accessioned2015-03-23T02:02:31Z-
dc.date.available2015-03-23T02:02:31Z-
dc.date.issued2011-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2011, v. 413, n. 3, p. 2235-2241-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/209002-
dc.description.abstractWe study the eccentricity distribution of a thick-disc sample of stars (defined as those withVy > 50kms-1and1 < |z|/kpc < 3) observed in the Radial Velocity Experiment (RAVE). We compare this distribution with those obtained in four simulations of galaxy formation taken from the literature as compiled by Sales et al. Each simulation emphasizes different scenarios for the origin of such stars (satellite accretion, heating of a pre-existing thin disc during a merger, radial migration, and gas-rich mergers). We find that the observed distribution peaks at low eccentricities and falls off smoothly and rather steeply to high eccentricities. This finding is fairly robust to changes in distances and to plausible assumptions about thin-disc contamination. Our results favour models where the majority of stars formed in the Galaxy itself on orbits of modest eccentricity and disfavour the pure satellite accretion case. A gas-rich merger origin where most of the stars form 'in situ' appears to be the most consistent with our data. © 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectSolar neighbourhood-
dc.subjectGalaxy: disc-
dc.subjectGalaxy: formation-
dc.subjectGalaxy: structure-
dc.titleTesting formation mechanisms of the Milky Way's thick disc with RAVE-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2011.18298.x-
dc.identifier.scopuseid_2-s2.0-79955787167-
dc.identifier.volume413-
dc.identifier.issue3-
dc.identifier.spage2235-
dc.identifier.epage2241-
dc.identifier.eissn1365-2966-

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