{
  "id": "1710.08098",
  "version": "v1",
  "published": "2017-10-23T05:50:40.000Z",
  "updated": "2017-10-23T05:50:40.000Z",
  "title": "The Hard X-ray emission of the blazar PKS 2155--304",
  "authors": [
    "Haritma Gaur",
    "Liang Chen",
    "R. Misra",
    "S. Sahayanathan",
    "M. F. Gu",
    "P. Kushwaha",
    "G. C. Dewangan"
  ],
  "comment": "14 pages, 7 Figures, Accepted for publication in ApJ",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "The synchrotron peak of the X-ray bright High Energy Peaked Blazar (HBL) PKS 2155$-$304 occurs in the UV-EUV region and hence its X-ray emission (0.6--10 keV) lies mostly in the falling part of the synchrotron hump. We aim to study the X-ray emission of PKS 2155$-$304 during different intensity states in 2009$-$2014 using XMM$-$Newton satellite. We studied the spectral curvature of all of the observations to provide crucial information on the energy distribution of the non-thermal particles. Most of the observations show curvature or deviation from a single power-law and can be well modeled by a log parabola model. In some of the observations, we find spectral flattening after 6 keV. In order to find the possible origin of the X-ray excess, we built the Multi-band Spectral Energy distribution (SED). We find that the X-ray excess in PKS 2155--304 is difficult to fit in the one zone model but, could be easily reconciled in the spine/layer jet structure. The hard X-ray excess can be explained by the inverse Comptonization of the synchrotron photons (from the layer) by the spine electrons.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-10-23T05:50:40.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "hard x-ray emission",
      "blazar pks",
      "bright high energy peaked blazar",
      "multi-band spectral energy distribution",
      "x-ray bright high energy"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 14,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}