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dc.contributor.authorNegueruela, I.
dc.contributor.authorMonguió, M.
dc.contributor.authorMarco, A.
dc.contributor.authorTabernero, H. M.
dc.contributor.authorGonzález-Fernández, C.
dc.contributor.authorDorda, R.
dc.date.accessioned2018-07-04T16:13:44Z
dc.date.available2018-07-04T16:13:44Z
dc.date.issued2018-07-01
dc.identifier.citationNegueruela , I , Monguió , M , Marco , A , Tabernero , H M , González-Fernández , C & Dorda , R 2018 , ' Berkeley 51, a young open cluster with four yellow supergiants ' , Monthly Notices of the Royal Astronomical Society , vol. 477 , no. 3 , pp. 2976-2990 . https://doi.org/10.1093/mnras/sty718
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/2299/20264
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
dc.description.abstractThe heavily obscured open cluster Berkeley 51 shows characteristics typical of young massive clusters, even though the few previous studies have suggested older ages.We combine optical (UBV) and 2MASS photometry of the cluster field with multi-object and long-slit optical spectroscopy for a large sample of stars. We apply classical photometric analysis techniques to determine the reddening to the cluster, and then derive cluster parameters via isochrone fitting. We find a large population of B-type stars, with a main-sequence turn-off at B3V, as well as a large number of supergiants with spectral types ranging from F to M. We use intermediate-resolution spectra of the evolved cool stars to derive their stellar parameters and find an essentially solar iron abundance. Under the plausible assumption that our photometry reaches stars still close to the zero-age main sequence, the cluster is located at d ≈ 5.5 kpc and has an age of ~60 Ma, though a slightly younger and more distant cluster cannot be ruled out. Despite the apparent good fit of isochrones, evolved stars seem to reside in positions of the colour-magnitude diagram far away from the locations where stellar tracks predict helium burning to occur. Of particular interest is the presence of four yellow supergiants, two on the ascending branch and two others close to or inside the instability strip.en
dc.format.extent15
dc.format.extent4925742
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectOpen clusters and associations: Individual: Berkeley 51
dc.subjectStars: Evolution
dc.subjectSupergiants
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleBerkeley 51, a young open cluster with four yellow supergiantsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85047130905&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1093/mnras/sty718
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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