{
  "id": "1801.03006",
  "version": "v1",
  "published": "2018-01-09T15:41:16.000Z",
  "updated": "2018-01-09T15:41:16.000Z",
  "title": "Evidence for the ultra-compact nature of IGR J17062-6143",
  "authors": [
    "J. V. Hernandez Santisteban",
    "V. Cuneo",
    "N. Degenaar",
    "J. van den Eijnden",
    "D. Altamirano",
    "M. N. Gomez",
    "D. M. Russell",
    "R. Wijnands",
    "R. Golovakova",
    "M. T. Reynolds",
    "J. M. Miller"
  ],
  "comment": "12 pages, 9 figures, submitted to MNRAS",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "We present a multi-wavelength study of the persistent low-luminosity neutron star low-mass X-ray binary \\igr. The multi-epoch photometric UV to NIR spectral energy distribution (SED) is consistent with an accretion disc $F_{\\nu}\\propto\\nu^{1/3}$. The SED modelling of the accretion disc allowed us to estimate an outer disc radius of $R_{out}=3.9^{+1.9}_{-1.1} \\times 10^{9}$ cm and a mass-transfer rate $\\dot{m}=1.7^{+6.9}_{-1.2}\\times10^{-9}$ M$_{\\odot}$ yr$^{-1}$, consistent with both theoretical and observational estimates of ultra-compact X-ray binaries (UCXB). In combination with empirical X-ray/NIR relationships, we estimate the orbital period of the system to be $\\sim0.4-1$ hr. In addition, we obtained a low-resolution optical spectrum which revealed a blue continuum and no emission lines. The lack of hydrogen in the spectrum and the size of the accretion disc provide further evidence for an ultra-compact nature of this system.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2018-01-09T15:41:16.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "ultra-compact nature",
      "accretion disc",
      "neutron star low-mass x-ray binary",
      "low-luminosity neutron star low-mass x-ray",
      "persistent low-luminosity neutron star low-mass"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 12,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}