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        FSR 1716: A new Milky Way Globular Cluster confirmed using VVV RR Lyrae stars

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        Author
        Minniti, Dante
        Palma, Tali
        Dékány, Istvan
        Hempel, Maren
        Rejkuba, Marina
        Pullen, Joyce
        Alonso-García, Javier
        Barbá, Rodolfo
        Barbuy, Beatriz
        Bica, Eduardo
        Bonatto, Charles
        Borissova, Jura
        Catelan, Marcio
        Carballo-Bello, Julio A.
        Chene, Andre Nicolas
        Clariá, Juan J.
        Cohen, Roger E.
        Contreras-Ramos, Rodrigo
        Dias, Bruno
        Emerson, Jim
        Froebrich, Dirk
        Buckner, Anne S. M.
        Geisler, Douglas
        Gonzalez, Oscar A.
        Gran, Felipe
        Hagdu, Gergely
        Irwin, Mike
        Ivanov, Valentin D.
        Kurtev, Radostin
        Lucas, Philip W.
        Majaess, Daniel
        Mauro, Francesco
        Moni-Bidin, Christian
        Navarrete, Camila
        Alegría, Sebastian Ramírez
        Saito, Roberto K.
        Valenti, Elena
        Zoccali, Manuela
        Attention
        2299/20634
        Abstract
        We 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.
        Publication date
        2017-03-24
        Published in
        Astrophysical Journal Letters
        Published version
        https://doi.org/10.3847/2041-8213/838/1/L14
        License
        Other
        Other links
        http://hdl.handle.net/2299/20634
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