{
  "id": "1805.00491",
  "version": "v1",
  "published": "2018-05-01T18:00:14.000Z",
  "updated": "2018-05-01T18:00:14.000Z",
  "title": "The Next Generation Fornax Survey (NGFS): IV. Mass and Age Bimodality of Nuclear Clusters in the Fornax Core Region",
  "authors": [
    "Y. Ordenes-Briceño",
    "T. H. Puzia",
    "P. Eigenthaler",
    "M. A. Taylor",
    "R. P. Muñoz",
    "H. Zhang",
    "K. Alamo-Martínez",
    "K. X. Ribbeck",
    "E. K. Grebel",
    "S. Ángel",
    "P. Côté",
    "L. Ferrarese",
    "M. Hilker",
    "A. Lançon",
    "S. Mieske",
    "B. W. Miller",
    "Y. Rong",
    "R. Sánchez-Janssen"
  ],
  "comment": "Accepted in ApJ, 21 pages, 12 figures, 3 tables",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We present the analysis of 61 nucleated dwarf galaxies in the central regions ($<R_{\\rm vir}/4$) of the Fornax galaxy cluster. The galaxies and their nuclei are studied as part of the Next Generation Fornax Survey (NGFS) using optical imaging obtained with the Dark Energy Camera (DECam) mounted at Blanco/CTIO and near-infrared data obtained with VIRCam at VISTA/ESO. We decompose the nucleated dwarfs in nucleus and spheroid, after subtracting the surface brightness profile of the spheroid component and studying the nucleus using PSF photometry.In general, nuclei are consistent with colors of confirmed metal-poor globular clusters, but with significantly smaller dispersion than other confirmed compact stellar systems in Fornax. We find a bimodal nucleus mass distribution with peaks located at $\\log({\\cal M_*}/M_\\odot)\\!\\simeq\\!5.4$ and $\\sim\\,6.3$. These two nucleus sub-populations have different stellar population properties, the more massive nuclei are older than $\\sim\\!2$ Gyr and have metal-poor stellar populations ($Z\\leq0.02\\,Z_\\odot$), while the less massive nuclei are younger than $\\sim\\!2$ Gyr with metallicities in the range $0.02\\!<\\!Z/Z_\\odot\\!\\leq\\!1$. We find that the nucleus mass (${\\cal M}_{\\rm nuc}$) vs. galaxy mass (${\\cal M}_{\\rm gal}$) relation becomes shallower for less massive galaxies starting around $10^8\\,M_\\odot$ and the mass ratio $\\eta_n\\!=\\!{\\cal M}_{\\rm nuc}/{\\cal M}_{\\rm gal}$ shows a clear anti-correlation with ${\\cal M}_{\\rm gal}$ for the lowest masses, reaching $10\\%$. We test current theoretical models of nuclear cluster formation and find that they cannot fully reproduce the observed trends. A likely mixture of in-situ star formation and star-cluster mergers seem to be acting during nucleus growth over cosmic time.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2018-05-01T18:00:14.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "generation fornax survey",
      "fornax core region",
      "nuclear cluster",
      "age bimodality",
      "bimodal nucleus mass distribution"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 21,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}