{
  "id": "2005.02401",
  "version": "v1",
  "published": "2020-05-05T18:00:01.000Z",
  "updated": "2020-05-05T18:00:01.000Z",
  "title": "The kinematics of globular cluster populations in the E-MOSAICS simulations and their implications for the assembly history of the Milky Way",
  "authors": [
    "Sebastian Trujillo-Gomez",
    "J. M. Diederik Kruijssen",
    "Marta Reina-Campos",
    "Joel L. Pfeffer",
    "Benjamin W. Keller",
    "Robert A. Crain",
    "Nate Bastian",
    "Meghan E. Hughes"
  ],
  "comment": "25 pages, 17 figures. Submitted to MNRAS",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We present a detailed comparison of the Milky Way (MW) globular cluster (GC) kinematics with the 25 Milky Way-mass cosmological simulations from the E-MOSAICS project. While the MW falls within the kinematic distribution of GCs spanned by the simulations, the relative kinematics of its metal-rich ($[\\rm{Fe/H}]>-1.2$) versus metal-poor ($[\\rm{Fe/H}]<-1.2$), and inner ($r<8\\rm{kpc}$) versus outer ($r>8\\rm{kpc}$) populations are atypical for its mass. To understand the origins of these features, we perform a comprehensive statistical analysis of the simulations, and find 18 correlations describing the assembly of $L^*$ galaxies and their dark matter haloes based on their GC population kinematics. The correlations arise because the orbital distributions of accreted and in-situ GCs depend on the masses and accretion redshifts of accreted satellites, driven by the combined effects of dynamical fraction, tidal stripping, and dynamical heating. Because the kinematics of in-situ/accreted GCs are broadly traced by the metal-rich/metal-poor and inner/outer populations, the observed GC kinematics are a sensitive probe of galaxy assembly. We predict that relative to the population of $L^*$ galaxies, the MW assembled its dark matter and stellar mass rapidly through a combination of in-situ star formation, more than a dozen low-mass mergers, and $1.4\\pm1.2$ early ($z=3.1\\pm1.3$) major merger. The rapid assembly period ended early, limiting the fraction of accreted stars. We conclude by providing detailed quantitative predictions for the assembly history of the MW.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2020-05-05T18:00:01.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "globular cluster populations",
      "assembly history",
      "e-mosaics simulations",
      "implications",
      "milky way-mass cosmological simulations"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 25,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}