Examinando por Autor "Piatti, A.E."

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  • Miniatura
    Ítem
    Candidate star clusters toward the inner Milky Way discovered on deep-stacked KS-band images from the VVV Survey
    (EDP Sciences, 2017) Ivanov, V.D.; Piatti, A.E.; Beamín, J.-C.; Minniti, D.; Borissova, J.; Kurtev, R.; Hempel, M.; Saito, R.K.
    This paper is based on observations made with ESO telescopes at the La Silla Paranal Observatory under program ID 092.B-0104(A). We have made extensive use of the SIMBAD Database at CDS (Centre de Données astronomiques) Strasbourg, the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, CalTech, under contract with NASA, and of the VizieR catalog access tool, CDS, Strasbourg, France. Support for J.B., D.M., J.C.B., R.K., M.H. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. Support for R.K. is provided from Fondecyt Reg. No. 1130140. R.K.S. acknowledges support from CNPq/Brazil through project 310636/2013-2. We are grateful to the anonymous referee for useful suggestions that helped to improve the paper.
  • Miniatura
    Ítem
    The VISCACHA survey-II. Structure of star clusters in the Magellanic Clouds periphery
    (Oxford University Press, 2020-10) Santos, J.F.C.; Maia, F.F.S.; Dias, B.; Kerber, L.D.O.; Piatti, A.E.; Bica, E.; Angelo, M.S.; Minniti, D.; Pérez-Villegas, A.; Roman-Lopes, A.; Westera, P.; Fraga L.
    We provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters' stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings. Integrated magnitudes and masses (for a subsample) are also provided. The sample contains mostly low surface brightness clusters with distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and SMC centres, respectively. We analysed their spatial distribution and structural properties, comparing them with those of inner clusters. Half-light and Jacobi radii were estimated, allowing an evaluation of the Roche volume tidal filling. We found that: (i) for our sample of LMC clusters, the tidal radii are, on average, larger than those of inner clusters from previous studies; (ii) the core radii dispersion tends to be greater for LMC clusters located towards the southwest, with position angles of ∼200° and about ∼5° from the LMC centre, i.e.Those LMC clusters nearer to the SMC; (iii) the core radius evolution for clusters with known age is similar to that of inner clusters; (iv) SMC clusters with galactocentric distances closer than 4 kpc are overfilling; (v) the recent Clouds collision did not leave marks on the LMC clusters' structure that our analysis could reveal. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.