{
  "id": "1512.01487",
  "version": "v1",
  "published": "2015-12-04T17:28:19.000Z",
  "updated": "2015-12-04T17:28:19.000Z",
  "title": "Inverting the dynamical evolution of globular clusters: clues to their origin",
  "authors": [
    "Mark Gieles",
    "Poul Alexander"
  ],
  "comment": "8 pages, 5 figures, invited review for IAUS 316, \"Formation, evolution, and survival of massive star clusters\", eds. C. Charbonnel & A. Nota",
  "categories": [
    "astro-ph.GA",
    "astro-ph.SR"
  ],
  "abstract": "Scaling relations for globular clusters (GC) differ from scaling relations for pressure supported (elliptical) galaxies. We show that two-body relaxation is the dominant mechanism in shaping the bivariate dependence of density on mass and Galactocentric distance for Milky Way GCs with masses <10^6 Msun, and it is possible, but not required, that GCs formed with similar scaling relations as ultra-compact dwarf galaxies. We use a fast cluster evolution model to fit a parameterised model for the initial properties of Milky Way GCs to the observed present-day properties. The best-fit cluster initial mass function is substantially flatter (power-law index alpha =- 0.6+/-0.2) than what is observed for young massive clusters (YMCs) forming in the nearby Universe (alpha =~-2). A slightly steeper CIMF is allowed when considering the metal-rich GCs separately (alpha =~-1.2+/-0.4$). If stellar mass loss and two-body relaxation in the Milky Way tidal field are the dominant disruption mechanisms, then GCs formed differently from YMCs.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-12-04T17:28:19.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "globular clusters",
      "dynamical evolution",
      "milky way gcs",
      "best-fit cluster initial mass function",
      "scaling relations"
    ],
    "tags": [
      "review article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 8,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}