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dc.contributor.authorHarris, A.
dc.contributor.authorDrew, J. E.
dc.contributor.authorMonguió, M.
dc.date.accessioned2019-07-29T11:01:22Z
dc.date.available2019-07-29T11:01:22Z
dc.date.issued2019-05-01
dc.identifier.citationHarris , A , Drew , J E & Monguió , M 2019 , ' A study of full space motions of outer Galactic disk A and F stars in two deep pencil beams ' , Monthly Notices of the Royal Astronomical Society , vol. 485 , no. 2 , stz442 , pp. 2312–2323 . https://doi.org/10.1093/mnras/stz442
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 16589697
dc.identifier.otherPURE UUID: 74ec1225-7faa-4a6e-8444-99396a259b2b
dc.identifier.otherArXiv: http://arxiv.org/abs/1902.04577v1
dc.identifier.otherScopus: 85067025959
dc.identifier.urihttp://hdl.handle.net/2299/21478
dc.description© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
dc.description.abstractA and F stars can be used as probes of outer Galactic disc kinematics: here we extend the work of Harris et al. by cross-matching their A/F sample with Gaia DR2 to bring in proper motions. These are combined with the already measured radial velocities and spectrophotometric distances to obtain full space motions. We use this sample of 1173 stars, located in two pencil-beam sightlines (ℓ = 178° and ℓ = 118°), to sample the Galactocentric velocity field out to almost RG = 15 kpc. We find there are significant differences in all three (radial, azimuthal, and vertical) kinematic components between the two directions. The rotation curve is roughly flat in the anticentre direction, confirming and extending the result of Kawata et al. thanks to the greater reach of our spectrophotometric distance scale. However at ℓ = 118° the circular velocity rises outwards from RG = 10.5 kpc and there is a more pronounced gradient in radial motion than is seen at ℓ = 178°. Furthermore, the A star radial motion differs from the F stars by ∼10 km s−1. We discuss our findings in the context of perturbers potentially responsible for the trends, such as the central bar, spiral arms, the warp, and external satellites. Our results at ℓ = 178° are broadly consistent with previous work on K giants in the anticentre, but the kinematics at ℓ = 118° in the Perseus region do not yet reconcile easily with bar or spiral arm perturbation.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectDynamics
dc.subjectGalaxy: disc
dc.subjectGalaxy: kinematics
dc.subjectMethods: observational
dc.subjectStars: early-type
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleA study of full space motions of outer Galactic disk A and F stars in two deep pencil beamsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85067025959&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2019-05-01
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stz442
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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