{
  "id": "1912.07652",
  "version": "v1",
  "published": "2019-12-16T19:32:01.000Z",
  "updated": "2019-12-16T19:32:01.000Z",
  "title": "First detection of the [OI] 63-um emission from a redshift 6 dusty galaxy",
  "authors": [
    "M. Rybak",
    "J. A Zavala",
    "J. A. Hodge",
    "C. M. Casey",
    "P. van der Werf"
  ],
  "comment": "Submitted to ApJL",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We report a ground-based detection of the [OI] 63-um line in a z=6.027 gravitationally lensed dusty star-forming galaxy (DSFG) G09.83808 using the APEX SEPIA 660 receiver, the first unambiguous detection of the [OI]63 line beyond redshift 3, and the first obtained from the ground. The [OI]63 line is robustly detected at 22$\\pm$5 Jy km s$^{-1}$, corresponding to an intrinsic (de-lensed) luminosity of $(5.4\\pm1.3)\\times10^{9}$ L$_\\odot$. With the [OI]63/[CII] luminosity ratio of 4, the [OI]63 line is the main coolant of the neutral gas in this galaxy, in agreement with model predictions. The high [OI]63 luminosity compensates for the pronounced [CII] deficit ([CII]/FIR$\\simeq4\\times10^{-4}$). Using photon-dominated region models, we derive a source-averaged gas density $n=10^{4.0}$ cm$^{-3}$, and far-UV field strength $G=10^4 G_0$, comparable to the z=2-4 DSFG population. If G09.83808 represents a typical high-redshift DSFG, the [OI]63 line from z=6 non-lensed DSFGs should be routinely detectable in ALMA Band 9 observations with $\\sim$15 min on-source, opening a new window to study the properties of the earliest DSFGs.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2019-12-16T19:32:01.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "first detection",
      "dusty galaxy",
      "far-uv field strength",
      "luminosity",
      "gravitationally lensed dusty star-forming galaxy"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}