{
  "id": "1504.04988",
  "version": "v1",
  "published": "2015-04-20T09:40:01.000Z",
  "updated": "2015-04-20T09:40:01.000Z",
  "title": "Formation of elongated galaxies with low masses at high redshift",
  "authors": [
    "Daniel Ceverino",
    "Joel Primack",
    "Avishai Dekel"
  ],
  "comment": "submitted to MNRAS letters, 6 pages, 3 figures",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "We report the identification of elongated (triaxial or prolate) galaxies in cosmological simulations at $z\\simeq2$. These are preferentially low-mass galaxies ($M_s \\le 10^{9.5} \\ M_\\odot$), residing in dark-matter (DM) haloes with strongly elongated inner parts, a common feature of high-redshift DM haloes in the $\\Lambda$CDM cosmology. Feedback slows formation of stars at the centres of these halos, so that a dominant and prolate DM distribution gives rise to galaxies elongated along the DM major axis. As galaxies grow in stellar mass, stars dominate the total mass within the galaxy half-mass radius, making stars and DM rounder and more oblate. A large population of elongated galaxies produces a very asymmetric distribution of projected axis ratios, as observed in high-z galaxy surveys. This indicates that the majority of the galaxies at high redshifts are not discs or spheroids but rather galaxies with elongated morphologies.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-04-20T09:40:01.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "high redshift",
      "low masses",
      "high-z galaxy surveys",
      "high-redshift dm haloes",
      "feedback slows formation"
    ],
    "publication": {
      "doi": "10.1093/mnras/stv1603"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1362154
    }
  }
}