{ "id": "1905.04330", "version": "v1", "published": "2019-05-10T18:22:13.000Z", "updated": "2019-05-10T18:22:13.000Z", "title": "Detection of Superluminal Motion in the X-ray Jet of M87", "authors": [ "Bradford Snios", "Paul E. J. Nulsen", "Ralph P. Kraft", "C. C. Cheung", "Eileen T. Meyer", "William R. Forman", "Christine Jones", "Stephen S. Murray" ], "comment": "Accepted to ApJ, 12 pages, 4 figures, 4 tables", "categories": [ "astro-ph.HE" ], "abstract": "Chandra HRC observations are investigated for evidence of proper motion and brightness changes in the X-ray jet of the nearby radio galaxy M87. Using images spanning 5 years, proper motion is measured in the X-ray knot HST-1, with a superluminal apparent speed of $6.3 \\pm 0.4 c$, or $24.1 \\pm 1.6\\rm\\ mas\\ yr^{-1}$, and in Knot D, with a speed of $2.4\\pm 0.6c$. Upper limits are placed on the speeds of the remaining jet features. The X-ray knot speeds are in excellent agreement with existing measurements in the radio, optical, and ultraviolet. Comparing the X-ray results with images from the Hubble Space Telescope indicates that the X-ray and optical/UV emitting regions co-move. The X-ray knots also vary by up to 73% in brightness, whereas there is no evidence of brightness changes in the optical/UV. Using the synchrotron cooling models, we determine lower limits on magnetic field strengths of $\\sim 420~\\mu \\rm G$ and $\\sim 230~\\mu \\rm G$ for HST-1 and Knot A, respectively, consistent with estimates of the equipartition fields. Together, these results lend strong support to the synchrotron cooling model for Knot HST-1, which requires that its superluminal motion reflects the speed of relativistic bulk flow in the jet.", "revisions": [ { "version": "v1", "updated": "2019-05-10T18:22:13.000Z" } ], "analyses": { "keywords": [ "x-ray jet", "superluminal motion", "synchrotron cooling model", "nearby radio galaxy m87", "proper motion" ], "note": { "typesetting": "TeX", "pages": 12, "language": "en", "license": "arXiv", "status": "editable" } } }