VEGAS-SSS. II. Comparing the globular cluster systems in NGC 3115 and NGC 1399 using VEGAS and FDS survey data. The quest for a common genetic heritage of globular cluster systems

Michele Cantiello, Raffaele D'Abrusco, Marilena Spavone, Maurizio Paolillo, Massimo Capaccioli, Luca Limatola, Aniello Grado, Enrica Iodice, Gabriella Raimondo, Nicola Napolitano, John P. Blakeslee, Enzo Brocato, Duncan A. Forbes, Michael Hilker, Steffen Mieske, Reynier Peletier, Glenn van de Ven, Pietro Schipani

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Abstract

We analyze the globular cluster (GC) systems in two very different galaxies, NGC 3115 and NGC 1399. With the papers of this series, we aim at highlighting common and different properties in the GC systems in galaxies covering a wide range of parameter space. We compare the GCs in NGC 3115 and NGC 1399 as derived from the analysis of one square degree u-, g-, and i-band images taken with the VST telescope as part of the VST early-type galaxy survey (VEGAS) and Fornax deep survey (FDS). We selected GC candidates using as reference the morpho-photometric and color properties of confirmed GCs. The surface density maps of GCs in NGC 3115 reveal a morphology similar to the light profile of field stars; the same is true when blue and red GCs are taken separately. The GC maps for NGC 1399 are richer in structure and confirm the existence of an intra-cluster GC component. We confirm the presence of a spatial offset in the NGC 1399 GC centroid and find that the centroid of the GCs for NGC 3115 coincides well with the galaxy center. Both GC systems show unambiguous color bimodality in (g - i) and (u - i); the color-color relations of the two GC systems are slightly different with NGC 3115 appearing more linear than NGC 1399. The azimuthal average of the radial density profiles in both galaxies reveals a larger spatial extent for the total GCs population with respect to the galaxy surface brightness profile. For both galaxies, the red GCs have radial density profiles compatible with the galaxy light profile, while the radial profiles for blue GCs are shallower. As for the specific frequency of GCs, SN, we find it is a factor of two higher in NGC 1399 than for NGC 3115; this is mainly the result of extra blue GCs. By inspecting the radial behavior of the specific frequency, SN(
Original languageEnglish
Article numberA93
Number of pages25
JournalAstronomy & astrophysics
Volume611
DOIs
Publication statusPublished - 1-Apr-2018

Keywords

  • galaxies: elliptical and lenticular
  • cD
  • galaxies: star clusters: general
  • galaxies: individual: NGC 1399
  • NGC 3115
  • galaxies: clusters: individual: Fornax
  • galaxies: evolution
  • galaxies: stellar content
  • EARLY-TYPE GALAXIES
  • FORNAX CLUSTER
  • ELLIPTIC GALAXIES
  • DWARF GALAXIES
  • COLOR DISTRIBUTIONS
  • LOCAL GROUP
  • METALLICITY DISTRIBUTION
  • FORMATION EFFICIENCIES
  • WASHINGTON PHOTOMETRY
  • STELLAR POPULATIONS
  • NGC3115 & NGC1399 VEGAS-SSS globular clusters

    Cantiello, M. (Contributor), D'Abrusco, R. (Contributor), Spavone, M. (Contributor), Paolillo, M. (Contributor), Capaccioli, M. (Contributor), Limatola, L. (Contributor), Grado, A. (Contributor), Iodice, E. (Contributor), Raimondo, G. (Contributor), Napolitano, N. (Contributor), Blakeslee, J. P. (Contributor), Brocato, E. (Contributor), Forbes, D. A. (Contributor), Hilker, M. (Contributor), Mieske, S. (Contributor), Peletier, R. (Contributor), Van De Ven, G. (Contributor) & Schipani, P. (Contributor), University of Groningen, 6-Apr-2018

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