{
  "id": "astro-ph/0012162",
  "version": "v1",
  "published": "2000-12-07T20:41:03.000Z",
  "updated": "2000-12-07T20:41:03.000Z",
  "title": "Structure of the X-ray Emission from the Jet of 3C 273",
  "authors": [
    "H. L. Marshall",
    "D. E. Harris",
    "J. P. Grimes",
    "J. J. Drake",
    "A. Fruscione",
    "M. Juda",
    "R. P. Kraft",
    "S. Mathur",
    "S. S. Murray",
    "P. M. Ogle",
    "D. O. Pease",
    "D. A. Schwartz",
    "A. L. Siemiginowska",
    "S. D. Vrtilek",
    "B. J. Wargelin"
  ],
  "comment": "10 pages, 5 figures; accepted for publication in the Astrophysical Journal Letters. For the color image, see fig1.ps or http://space.mit.edu/~hermanm/papers/3c273/fig1.jpg",
  "doi": "10.1086/319161",
  "categories": [
    "astro-ph"
  ],
  "abstract": "We present images from five observations of the quasar 3C 273 with the Chandra X-ray Observatory. The jet has at least four distinct features which are not resolved in previous observations. The first knot in the jet (A1) is very bright in X-rays. Its X-ray spectrum is well fitted with a power law with alpha = 0.60 +/- 0.05. Combining this measurement with lower frequency data shows that a pure synchrotron model can fit the spectrum of this knot from 1.647 GHz to 5 keV (over nine decades in energy) with alpha = 0.76 +/- 0.02, similar to the X-ray spectral slope. Thus, we place a lower limit on the total power radiated by this knot of 1.5e43 erg/s; substantially more power may be emitted in the hard X-ray and gamma-ray bands. Knot A2 is also detected and is somewhat blended with knot B1. Synchrotron emission may also explain the X-ray emission but a spectral bend is required near the optical band. For knots A1 and B1, the X-ray flux dominates the emitted energy. For the remaining optical knots (C through H), localized X-ray enhancements that might correspond to the optical features are not clearly resolved. The position angle of the jet ridge line follows the optical shape with distinct, aperiodic excursions of +/-1 deg from a median value of -138.0deg. Finally, we find X-ray emission from the ``inner jet'' between 5 and 10\" from the core.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2000-12-07T20:41:03.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "x-ray emission",
      "chandra x-ray observatory",
      "jet ridge line",
      "lower frequency data",
      "x-ray flux dominates"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 10,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 549026
    }
  }
}