2004/07/16 by D. E. Harris, A. E. Mossman, R. C. Walker · 3 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #astro-ph
paper · pdf · doi:10.1086/424442
published as Astrophys.J. 615 (2004) 161-172 · Accepted for publication in the Astrophysical Journal (tentatively scheduled for the ApJ 1 November 2004, v615 issue). 18 pages including 9 figures. Figs 1, 2, 3, 4, and 8 are jpegs to limit the size of the files. Figs 4 and 8 are in color
arxiv created 2004/07/16 · openalex publication_date 2004/11/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We report on archival data from the Chandra X-Ray Observatory for the radio jet of 3C 120. We consider the emission process responsible for the X-rays from four knots using spectra constructed from radio, optical, and X-ray intensities. While a simple synchrotron model is adequate for three of the knots, the fourth ("k25"), which was previously detected by ROSAT and is now well resolved with Chandra , still represents a problem for the conventional emission processes. If, as we argue, the flat X-ray spectra from two parts of k25 are synchrotron emission, then it appears that either the emission comes from an electron distribution spectrally distinct from that responsible for the radio emission or at the highest electron energies there is a significant deviation from the power law describing the electron distribution at lower energies.