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dc.contributor.authorChengyan, Li
dc.contributor.authorde Grijs, R.
dc.contributor.authorDeng, Licai
dc.contributor.authorRubele, S.
dc.contributor.authorWang, Chuchu
dc.contributor.authorBekki, K.
dc.contributor.authorCioni, M-R.L.
dc.contributor.authorClementini, G.
dc.contributor.authorEmerson, J.P.
dc.contributor.authorFor, Bi-Qing
dc.contributor.authorGirardi, L.
dc.contributor.authorGroenewegen, M.A.T.
dc.contributor.authorGuandalini, Roald
dc.contributor.authorGullieuszik, M.
dc.contributor.authorMarconi, M.
dc.contributor.authorPiatti, Andres
dc.contributor.authorRipepi, V.
dc.contributor.authorvan Loon, J. Th.
dc.date.accessioned2014-09-25T08:15:58Z
dc.date.available2014-09-25T08:15:58Z
dc.date.issued2014-07
dc.identifier.citationChengyan , L , de Grijs , R , Deng , L , Rubele , S , Wang , C , Bekki , K , Cioni , M-RL , Clementini , G , Emerson , J P , For , B-Q , Girardi , L , Groenewegen , M A T , Guandalini , R , Gullieuszik , M , Marconi , M , Piatti , A , Ripepi , V & van Loon , J T 2014 , ' The VMC survey - XI : Radial Stellar Population Gradients in the Galactic Globular Cluster 47 Tucanae ' , The Astrophysical Journal , vol. 790 , no. 1 , 35 . https://doi.org/10.1088/0004-637X/790/1/35
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 7416303
dc.identifier.otherPURE UUID: 1fb5e358-b547-48d7-8843-b2f6e26e8680
dc.identifier.otherScopus: 84904198530
dc.identifier.urihttp://hdl.handle.net/2299/14476
dc.descriptionCopyright American Astronomical Society
dc.description.abstractWe present a deep near-infrared color-magnitude diagram of the Galactic globular cluster 47 Tucanae, obtained with the Visible and Infrared Survey Telescope for Astronomy (VISTA) as part of the VISTA near-infrared Y, J, Ks survey of the Magellanic System (VMC). The cluster stars comprising both the subgiant and red giant branches exhibit apparent, continuous variations in color-magnitude space as a function of radius. Subgiant branch stars at larger radii are systematically brighter than their counterparts closer to the cluster core; similarly, red-giant-branch stars in the cluster's periphery are bluer than their more centrally located cousins. The observations can very well be described by adopting an age spread of ~0.5 Gyr as well as radial gradients in both the cluster's helium abundance (Y) and metallicity (Z), which change gradually from (Y = 0.28, Z = 0.005) in the cluster core to (Y = 0.25, Z = 0.003) in its periphery. We conclude that the cluster's inner regions host a significant fraction of second-generation stars, which decreases with increasing radius; the stellar population in the 47 Tuc periphery is well approximated by a simple stellar population.en
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.titleThe VMC survey - XI : Radial Stellar Population Gradients in the Galactic Globular Cluster 47 Tucanaeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2014-07
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/790/1/35
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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