{
  "id": "2212.13946",
  "version": "v1",
  "published": "2022-12-28T16:47:10.000Z",
  "updated": "2022-12-28T16:47:10.000Z",
  "title": "Star Cluster Formation and Survival in the First Galaxies",
  "authors": [
    "Fred Angelo Batan Garcia",
    "Massimo Ricotti",
    "Kazuyuki Sugimura",
    "Jongwon Park"
  ],
  "comment": "20 pages, 15 figures, submitted to MNRAS. See https://fred144.github.io/research.html for movie renders",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "Using radiation-hydrodynamic cosmological simulations, we present a detailed ($0.1$ pc resolution), physically motivated portrait of a typical-mass dwarf galaxy before the epoch of reionization, resolving the formation and evolution of star clusters into individual $10\\:\\mathrm{M_{\\odot}}$ star particles. In the rest-frame UV, the galaxy has an irregular morphology with no bulge or galactic disk, dominated by light emitted from numerous, compact, and gravitationally-bound star clusters. This is especially interesting in light of recent HST and JWST observations that -- aided by the magnifying power of gravitational lenses -- have imaged, at parsec-scale resolution, individual young star clusters in the process of forming in similar galaxies at $z>6$. Because of their low metallicities and high temperatures, star-forming gas clouds in this galaxy have densities $\\sim 100$ times higher than typical giant molecular clouds; hence, their star formation efficiencies are high enough ($f_*\\sim10-70$ per cent) to produce a sizeable population of potential globular cluster progenitors but typically smaller (between a few $100\\:-\\: 2\\times10^4\\:\\mathrm{M_{\\odot}}$, sizes of $0.1-3$ pc) and of lower metallicities ($10^{-3.5}-10^{-2.5}\\:\\mathrm{Z_{\\odot}}$). The initial mass function of the star-forming clouds is log-normal while the bound star cluster mass function is a power-law with a slope that depends mainly on $f_*$ but also on the temporal proximity to a major starburst. We find slopes between $-0.5$ and $-2.5$ depending on the assumed sub-grid $f_*$. Star formation is self-regulated on galactic scales; however, the multi-modal metallicity distribution of the star clusters and the fraction of stars locked into surviving bound star clusters depends on $f_*$.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-12-28T16:47:10.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "star cluster formation",
      "first galaxies",
      "bound star cluster mass function",
      "potential globular cluster progenitors",
      "star formation"
    ],
    "tags": [
      "github project"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 20,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}