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^★

¹ INAF Osservatorio Astr. di Teramo, via Maggini, 64100 Teramo, Italy
e-mail: cantiello@oa-teramo.inaf.it
² Smithsonian Astrophysical Observatory, 60 Garden Street, 02138 Cambridge, MA, USA
³ INAF Osservatorio Astr. di Capodimonte Napoli, Salita Moiariello, 80131 Napoli, Italy
⁴ Dip. di Fisica, Universitá di Napoli Federico II, C.U. di Monte Sant’Angelo, via Cintia, 80126 Naples, Italy
⁵ NRC Herzberg Astronomy & Astrophysics, Victoria, BC V9E 2E7, Canada
⁶ INAF Osservatorio Astronomico di Roma, via di Frascati, 33, 00040 Monteporzio Catone, Italy
⁷ Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC 3122, Australia
⁸ European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
⁹ European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
¹⁰ Kapteyn Astronomical Institute, University of Groningen, PO Box 72, 9700 AV Groningen, The Netherlands
¹¹ Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany

Received: 17 February 2017
Accepted: 16 October 2017

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, S_N, 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, S_N(<r), for the total, blue, and red GCs, we find notable similarities between the trends for red GCs in the two targets. In spite of extremely different host environments, the red GCs in both cases appear closely linked to the light distribution of field stars. Blue GCs extend to larger galactocentric scales than red GCs, marking a significant difference between the two galaxies: the blue/red GCs and field stellar components of NGC 3115 appear well thermalized with each other and the blue GCs in NGC 1399 appear to fade into an unrelaxed intra-cluster GC population.