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Article: The imprints of the galactic bar on the thick disk with rave

TitleThe imprints of the galactic bar on the thick disk with rave
Authors
KeywordsGalaxy: disk
Galaxy: kinematics and dynamics
Galaxy: structure
Issue Date2015
Citation
Astrophysical Journal Letters, 2015, v. 800, n. 2 How to Cite?
Abstract© 2015. The American Astronomical Society. All rights reserved. We study the kinematics of a local sample of stars, located within a cylinder of 500 pc radius centered on the Sun, in the RAVE data set. We find clear asymmetries in the vR v∞ velocity distributions of thin and thick disk stars: there are more stars moving radially outward for low azimuthal velocities and more radially inward for high azimuthal velocities. Such asymmetries have been previously reported for the thin disk as being due to the Galactic bar, but this is the first time that the same type of structures are seen in the thick disk. Our findings imply that the velocities of thick-disk stars should no longer be described by Schwarzschilds, multivariate Gaussian or purely axisymmetric distributions. Furthermore, the nature of previously reported substructures in the thick disk needs to be revisited as these could be associated with dynamical resonances rather than to accretion events. It is clear that dynamical models of the Galaxy must fit the 3D velocity distributions of the disks, rather than the projected 1D, if we are to understand the Galaxy fully.
Persistent Identifierhttp://hdl.handle.net/10722/209048
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorAntoja, Teresa-
dc.contributor.authorMonari, G.-
dc.contributor.authorHelmi, Amina-
dc.contributor.authorBienaymé, Olivier-
dc.contributor.authorBland-Hawthorn, Joss Bland-
dc.contributor.authorFamaey, Benoît-
dc.contributor.authorGibson, B. K.-
dc.contributor.authorGrebel, Eva K.-
dc.contributor.authorKordopatis, Georges-
dc.contributor.authorMunari, Ulisse-
dc.contributor.authorNavarro, J.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorReid, Warren A.-
dc.contributor.authorSeabroke, George M.-
dc.contributor.authorSteinmetz, Matthias-
dc.contributor.authorZwitter, Tomaž-
dc.date.accessioned2015-03-23T02:31:18Z-
dc.date.available2015-03-23T02:31:18Z-
dc.date.issued2015-
dc.identifier.citationAstrophysical Journal Letters, 2015, v. 800, n. 2-
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/10722/209048-
dc.description.abstract© 2015. The American Astronomical Society. All rights reserved. We study the kinematics of a local sample of stars, located within a cylinder of 500 pc radius centered on the Sun, in the RAVE data set. We find clear asymmetries in the vR v∞ velocity distributions of thin and thick disk stars: there are more stars moving radially outward for low azimuthal velocities and more radially inward for high azimuthal velocities. Such asymmetries have been previously reported for the thin disk as being due to the Galactic bar, but this is the first time that the same type of structures are seen in the thick disk. Our findings imply that the velocities of thick-disk stars should no longer be described by Schwarzschilds, multivariate Gaussian or purely axisymmetric distributions. Furthermore, the nature of previously reported substructures in the thick disk needs to be revisited as these could be associated with dynamical resonances rather than to accretion events. It is clear that dynamical models of the Galaxy must fit the 3D velocity distributions of the disks, rather than the projected 1D, if we are to understand the Galaxy fully.-
dc.languageeng-
dc.relation.ispartofAstrophysical Journal Letters-
dc.subjectGalaxy: disk-
dc.subjectGalaxy: kinematics and dynamics-
dc.subjectGalaxy: structure-
dc.titleThe imprints of the galactic bar on the thick disk with rave-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/2041-8205/800/2/L32-
dc.identifier.scopuseid_2-s2.0-84923701399-
dc.identifier.volume800-
dc.identifier.issue2-
dc.identifier.eissn2041-8213-

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