{
  "id": "1801.07517",
  "version": "v1",
  "published": "2018-01-23T12:53:35.000Z",
  "updated": "2018-01-23T12:53:35.000Z",
  "title": "Persistent X-ray emission from ASASSN-15lh: pre-SLSN dense wind?",
  "authors": [
    "Yan Huang",
    "Zhuo Li"
  ],
  "comment": "6 pages, 3 figures and 1 table. Comments welcome",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "The persistent soft X-ray emission at the location of the so-far most luminous supernova (SN), ASASSN-15lh (or SN 2015L), with $L \\sim 10^{42} \\rm erg~ s^{-1}$, is puzzling. We show that it can be explained by radiation from the SN-shock accelerated electrons inverse-Compton scattering the intense UV photons. In this interpretation, the circumstellar medium is derived to be a wind ($n\\propto R^{-2}$) with mass-loss rate of $\\dot M \\gtrsim 3 \\times10^{-3}M_\\odot(v_{\\rm w}/10^3 \\rm km\\,s^{-1}) yr^{-1}$, and the initial velocity of the bulk SN ejecta is $\\lesssim0.03c$. The non-detection in radio is naturally expected due to strong synchrotron self-absorption and free-free absorption in the dense medium. This constraint implies a strong wind ejected just within $\\sim10(v_{\\rm w}/10^3 \\rm km\\,s^{-1})^{-1}$ yrs before the explosion of ASASSN-15lh by its progenitor star.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2018-01-23T12:53:35.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "pre-slsn dense wind",
      "persistent x-ray emission",
      "asassn-15lh",
      "accelerated electrons inverse-compton scattering",
      "persistent soft x-ray emission"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}