{
  "id": "2204.13140",
  "version": "v1",
  "published": "2022-04-27T18:24:17.000Z",
  "updated": "2022-04-27T18:24:17.000Z",
  "title": "Termination Shocks and the Extended X-ray Emission in MRK 78",
  "authors": [
    "Francesca M. Fornasini",
    "Martin Elvis",
    "W. Peter Maksym",
    "Giuseppina Fabbiano",
    "Thaisa Storchi Bergmann",
    "Poshak Gandhi",
    "Mark Whittle"
  ],
  "comment": "23 pages, 14 figures, 6 tables",
  "categories": [
    "astro-ph.HE",
    "astro-ph.GA"
  ],
  "abstract": "Sub-arcsecond imaging of the X-ray emission in the type 2 AGN Mrk 78 with Chandra shows complex structure with spectral variations on scales from $\\sim$200 pc to $\\sim$ 2 kpc. Overall the X-ray emission is aligned E-W with the radio (3.6 cm) and narrow emission line region as mapped in [OIII], with a marked E-W asymmetry. The Eastern X-ray emission is mostly in a compact knot coincident with the location where the radio source is deflected, while the Western X-ray emission forms a loop or shell $\\sim$2 kpc from the nucleus with radius $\\sim$0.7 kpc. There is suggestive evidence of shocks in both the Eastern knot and the Western arc. Both these positions coincide with large changes in the velocities of the [OIII] outflow. We discuss possible reasons why the X-ray shocks on the Western side occur $\\sim1$ kpc farther out than on the Eastern side. We estimate that the thermal energy injected by the shocks into the interstellar medium corresponds to $0.05-0.6$% of the AGN bolometric luminosity.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-04-27T18:24:17.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "extended x-ray emission",
      "termination shocks",
      "narrow emission line region",
      "compact knot coincident",
      "western x-ray emission forms"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 23,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}