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dc.contributor.authorMinniti, Dante
dc.contributor.authorPalma, Tali
dc.contributor.authorDékány, Istvan
dc.contributor.authorHempel, Maren
dc.contributor.authorRejkuba, Marina
dc.contributor.authorPullen, Joyce
dc.contributor.authorAlonso-García, Javier
dc.contributor.authorBarbá, Rodolfo
dc.contributor.authorBarbuy, Beatriz
dc.contributor.authorBica, Eduardo
dc.contributor.authorBonatto, Charles
dc.contributor.authorBorissova, Jura
dc.contributor.authorCatelan, Marcio
dc.contributor.authorCarballo-Bello, Julio A.
dc.contributor.authorChene, Andre Nicolas
dc.contributor.authorClariá, Juan J.
dc.contributor.authorCohen, Roger E.
dc.contributor.authorContreras-Ramos, Rodrigo
dc.contributor.authorDias, Bruno
dc.contributor.authorEmerson, Jim
dc.contributor.authorFroebrich, Dirk
dc.contributor.authorBuckner, Anne S. M.
dc.contributor.authorGeisler, Douglas
dc.contributor.authorGonzalez, Oscar A.
dc.contributor.authorGran, Felipe
dc.contributor.authorHagdu, Gergely
dc.contributor.authorIrwin, Mike
dc.contributor.authorIvanov, Valentin D.
dc.contributor.authorKurtev, Radostin
dc.contributor.authorLucas, Philip W.
dc.contributor.authorMajaess, Daniel
dc.contributor.authorMauro, Francesco
dc.contributor.authorMoni-Bidin, Christian
dc.contributor.authorNavarrete, Camila
dc.contributor.authorAlegría, Sebastian Ramírez
dc.contributor.authorSaito, Roberto K.
dc.contributor.authorValenti, Elena
dc.contributor.authorZoccali, Manuela
dc.date.accessioned2018-09-22T09:12:23Z
dc.date.available2018-09-22T09:12:23Z
dc.date.issued2017-03-24
dc.identifier.citationMinniti , D , Palma , T , Dékány , I , Hempel , M , Rejkuba , M , Pullen , J , Alonso-García , J , Barbá , R , Barbuy , B , Bica , E , Bonatto , C , Borissova , J , Catelan , M , Carballo-Bello , J A , Chene , A N , Clariá , J J , Cohen , R E , Contreras-Ramos , R , Dias , B , Emerson , J , Froebrich , D , Buckner , A S M , Geisler , D , Gonzalez , O A , Gran , F , Hagdu , G , Irwin , M , Ivanov , V D , Kurtev , R , Lucas , P W , Majaess , D , Mauro , F , Moni-Bidin , C , Navarrete , C , Alegría , S R , Saito , R K , Valenti , E & Zoccali , M 2017 , ' FSR 1716: A new Milky Way Globular Cluster confirmed using VVV RR Lyrae stars ' , Astrophysical Journal Letters , vol. 838 , no. 1 , L14 . https://doi.org/10.3847/2041-8213/838/1/L14
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 13277724
dc.identifier.otherPURE UUID: 187e8cf0-ac6a-40b8-a209-4faa989b7789
dc.identifier.otherArXiv: http://arxiv.org/abs/1703.02033v1
dc.identifier.otherScopus: 85016158900
dc.identifier.otherORCID: /0000-0002-8872-4462/work/62748903
dc.identifier.urihttp://hdl.handle.net/2299/20634
dc.description7 pages, 4 figures. © 2017. The American Astronomical Society. All rights reserved.
dc.description.abstractWe use deep multi-epoch near-IR images of the VISTA Variables in the V\'ia L\'actea (VVV) Survey to search for RR Lyrae stars towards the Southern Galactic plane. Here we report the discovery of a group of RR Lyrae stars close together in VVV tile d025. Inspection of the VVV images and PSF photometry reveals that most of these stars are likely to belong to a globular cluster, that matches the position of the previously known star cluster FSR\,1716. The stellar density map of the field yields a $>100$ sigma detection for this candidate globular cluster, that is centered at equatorial coordinates $RA_{J2000}=$16:10:30.0, $DEC_{J2000}=-$53:44:56; and galactic coordinates $l=$329.77812, $b=-$1.59227. The color-magnitude diagram of this object reveals a well populated red giant branch, with a prominent red clump at $K_s=13.35 \pm 0.05$, and $J-K_s=1.30 \pm 0.05$. We present the cluster RR Lyrae positions, magnitudes, colors, periods and amplitudes. The presence of RR Lyrae indicates an old globular cluster, with age $>10$ Gyr. We classify this object as an Oosterhoff type I globular cluster, based on the mean period of its RR Lyrae type ab, $ =0.540$ days, and argue that this is a relatively metal-poor cluster with $[Fe/H] = -1.5 \pm 0.4$ dex. The mean extinction and reddening for this cluster are $A_{K_s}=0.38 \pm 0.02$, and $E(J-K_s)=0.72 \pm 0.02$ mag, respectively, as measured from the RR Lyrae colors and the near-IR color-magnitude diagram. We also measure the cluster distance using the RR Lyrae type ab stars. The cluster mean distance modulus is $(m-M)_0 = 14.38 \pm 0.03$ mag, implying a distance $D = 7.5 \pm 0.2$ kpc, and a Galactocentric distance $R_G=4.3$ kpc.en
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Letters
dc.rightsEmbargoed
dc.subjectastro-ph.GA
dc.subjectastro-ph.SR
dc.titleFSR 1716: A new Milky Way Globular Cluster confirmed using VVV RR Lyrae starsen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.date.embargoedUntil2018-03-20
dc.identifier.urlhttps://arxiv.org/abs/1703.02033
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2017-03-24
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.3847/2041-8213/838/1/L14
rioxxterms.licenseref.uriOther
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeEmbargoed


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