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A dynamically young and perturbed Milky Way disk

hal.structure.identifierInstitut de Ciencies del Cosmos [ICCUB]
dc.contributor.authorANTOJA, T.
hal.structure.identifierKapteyn Astronomical Institute [Groningen]
dc.contributor.authorHELMI, A.
hal.structure.identifierInstitut de Ciencies del Cosmos [ICCUB]
dc.contributor.authorROMERO-GOMEZ, M.
hal.structure.identifierGalaxies, Etoiles, Physique, Instrumentation [GEPI]
dc.contributor.authorKATZ, D.
hal.structure.identifierGalaxies, Etoiles, Physique, Instrumentation [GEPI]
dc.contributor.authorBABUSIAUX, C.
hal.structure.identifierINAF - Osservatorio Astrofisico di Torino [OATo]
dc.contributor.authorDRIMMEL, R.
hal.structure.identifierInstitute of Astronomy [Cambridge]
dc.contributor.authorEVANS, D.
hal.structure.identifierInstitut de Ciencies del Cosmos [ICCUB]
dc.contributor.authorFIGUERAS, F.
hal.structure.identifierINAF - Osservatorio Astrofisico di Torino [OATo]
dc.contributor.authorPOGGIO, E.
hal.structure.identifierUnivers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) [UTINAM]
dc.contributor.authorREYLÉ, C.
hal.structure.identifierUnivers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) [UTINAM]
dc.contributor.authorROBIN, A.C.
hal.structure.identifierMullard Space Science Laboratory [MSSL]
dc.contributor.authorSEABROKE, G.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSOUBIRAN, C.
dc.date.issued2018-09
dc.identifier.issn0028-0836
dc.description.abstractEnThe evolution of the Milky Way disk, which contains most of the stars in the Galaxy, is affected by several phenomena. For example, the bar and the spiral arms of the Milky Way induce radial migration of stars1 and can trap or scatter stars close to orbital resonances2. External perturbations from satellite galaxies can also have a role, causing dynamical heating of the Galaxy3, ring-like structures in the disk4 and correlations between different components of the stellar velocity5. These perturbations can also cause ‘phase wrapping’ signatures in the disk6–9, such as arched velocity structures in the motions of stars in the Galactic plane. Some manifestations of these dynamical processes have already been detected, including kinematic substructure in samples of nearby stars10–12, density asymmetries and velocities across the Galactic disk that differ from the axisymmetric and equilibrium expectations13, especially in the vertical direction11,14–16, and signatures of incomplete phase mixing in the disk7,12,17,18. Here we report an analysis of the motions of six million stars in the Milky Way disk. We show that the phase- space distribution contains different substructures with various morphologies, such as snail shells and ridges, when spatial and velocity coordinates are combined. We infer that the disk must have been perturbed between 300 million and 900 million years ago, consistent with estimates of the previous pericentric passage of the Sagittarius dwarf galaxy. Our findings show that the Galactic disk is dynamically young and that modelling it as time-independent and axisymmetric is incorrect.
dc.language.isoen
dc.publisherNature Publishing Group
dc.title.enA dynamically young and perturbed Milky Way disk
dc.typeArticle de revue
dc.identifier.doi10.1038/s41586-018-0510-7
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1804.10196
bordeaux.journalNature
bordeaux.page360 - 362
bordeaux.volume561
bordeaux.issue7723
bordeaux.peerReviewedoui
hal.identifierhal-01878376
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01878376v1
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