File Download
There are no files associated with this item.
Links for fulltext
(May Require Subscription)
- Publisher Website: 10.1111/j.1365-2966.2011.18298.x
- Scopus: eid_2-s2.0-79955787167
- WOS: WOS:000290487700060
- Find via
Supplementary
- Citations:
- Appears in Collections:
Article: Testing formation mechanisms of the Milky Way's thick disc with RAVE
Title | Testing formation mechanisms of the Milky Way's thick disc with RAVE |
---|---|
Authors | Wilson, Michelle L.Helmi, AminaMorrison, Heather L.Breddels, Maarten A.Bienaymé, OlivierBinney, James J.Bland-Hawthorn, Joss BlandCampbell, Randy D.Freeman, Kenneth C.Fulbright, Jon P.Gibson, Brad K.Gilmore, Gerard F.Grebel, Eva K.Munari, UlisseNavarro, Julio F.Parker, Quentin A.Reid, Warren A.Seabroke, George M.Siebert, ArnaudSiviero, AlessandroSteinmetz, MatthiasWilliams, Mary E KWyse, Rosemary F GZwitter, Tomaž |
Keywords | Solar neighbourhood Galaxy: disc Galaxy: formation Galaxy: structure |
Issue Date | 2011 |
Citation | Monthly Notices of the Royal Astronomical Society, 2011, v. 413, n. 3, p. 2235-2241 How to Cite? |
Abstract | We 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 Identifier | http://hdl.handle.net/10722/209002 |
ISSN | 2023 Impact Factor: 4.7 2023 SCImago Journal Rankings: 1.621 |
ISI Accession Number ID |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Wilson, Michelle L. | - |
dc.contributor.author | Helmi, Amina | - |
dc.contributor.author | Morrison, Heather L. | - |
dc.contributor.author | Breddels, Maarten A. | - |
dc.contributor.author | Bienaymé, Olivier | - |
dc.contributor.author | Binney, James J. | - |
dc.contributor.author | Bland-Hawthorn, Joss Bland | - |
dc.contributor.author | Campbell, Randy D. | - |
dc.contributor.author | Freeman, Kenneth C. | - |
dc.contributor.author | Fulbright, Jon P. | - |
dc.contributor.author | Gibson, Brad K. | - |
dc.contributor.author | Gilmore, Gerard F. | - |
dc.contributor.author | Grebel, Eva K. | - |
dc.contributor.author | Munari, Ulisse | - |
dc.contributor.author | Navarro, Julio F. | - |
dc.contributor.author | Parker, Quentin A. | - |
dc.contributor.author | Reid, Warren A. | - |
dc.contributor.author | Seabroke, George M. | - |
dc.contributor.author | Siebert, Arnaud | - |
dc.contributor.author | Siviero, Alessandro | - |
dc.contributor.author | Steinmetz, Matthias | - |
dc.contributor.author | Williams, Mary E K | - |
dc.contributor.author | Wyse, Rosemary F G | - |
dc.contributor.author | Zwitter, Tomaž | - |
dc.date.accessioned | 2015-03-23T02:02:31Z | - |
dc.date.available | 2015-03-23T02:02:31Z | - |
dc.date.issued | 2011 | - |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society, 2011, v. 413, n. 3, p. 2235-2241 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.uri | http://hdl.handle.net/10722/209002 | - |
dc.description.abstract | We 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.language | eng | - |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | - |
dc.subject | Solar neighbourhood | - |
dc.subject | Galaxy: disc | - |
dc.subject | Galaxy: formation | - |
dc.subject | Galaxy: structure | - |
dc.title | Testing formation mechanisms of the Milky Way's thick disc with RAVE | - |
dc.type | Article | - |
dc.description.nature | link_to_OA_fulltext | - |
dc.identifier.doi | 10.1111/j.1365-2966.2011.18298.x | - |
dc.identifier.scopus | eid_2-s2.0-79955787167 | - |
dc.identifier.volume | 413 | - |
dc.identifier.issue | 3 | - |
dc.identifier.spage | 2235 | - |
dc.identifier.epage | 2241 | - |
dc.identifier.eissn | 1365-2966 | - |
dc.identifier.isi | WOS:000290487700060 | - |
dc.identifier.issnl | 0035-8711 | - |