{
  "id": "2103.12705",
  "version": "v1",
  "published": "2021-03-23T17:25:15.000Z",
  "updated": "2021-03-23T17:25:15.000Z",
  "title": "The dust mass in Cassiopeia A from infrared and optical line flux differences",
  "authors": [
    "Maria Niculescu-Duvaz",
    "Michael J. Barlow",
    "Antonia Bevan",
    "Danny Milisavljevic",
    "Ilse De Looze"
  ],
  "comment": "14 pages,12 figures, will appear in MNRAS",
  "categories": [
    "astro-ph.GA",
    "astro-ph.SR"
  ],
  "abstract": "The large quantities of dust that have been found in a number of high redshift galaxies have led to suggestions that core-collapse supernovae (CCSNe) are the main sources of their dust and have motivated the measurement of the dust masses formed by local CCSNe. For Cassiopeia~A, an oxygen-rich remnant of a Type~IIb CCSN, a dust mass of 0.6-1.1~M$_\\odot$ has already been determined by two different methods, namely (a) from its far-infrared spectral energy distribution and (b) from analysis of the red-blue emission line asymmetries in its integrated optical spectrum. We present a third, independent, method for determining the mass of dust contained within Cas~A. This compares the relative fluxes measured in similar apertures from [O~{\\sc iii}] far-infrared and visual-region emission lines, taking into account foreground dust extinction, in order to determine internal dust optical depths, from which corresponding dust masses can be obtained. Using this method we determine a dust mass within Cas~A of at least 0.99$^{+0.10}_{-0.09}$~M$_\\odot$.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-03-23T17:25:15.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "dust mass",
      "optical line flux differences",
      "determine internal dust optical depths",
      "account foreground dust extinction",
      "cassiopeia"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 14,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}