Structure of the X-Ray Emission from the Jet of 3C 273
Murray, S. S.; Mathur, S.; Drake, J. J.; Schwartz, D. A.; Marshall, H. L.; Fruscione, A.; Kraft, R. P.; Vrtilek, S. D.; Harris, D. E.; Ogle, P. M.; Grimes, J. P.; Juda, M.; Pease, D. O.; Siemiginowska, A. L.; Wargelin, B. J.
United States
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 that 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 α=0.60+/-0.05 (where Sν~ν-α). 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 α=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 1.5×1043 ergs s-1 substantially more power may be emitted in the hard X-ray and γ-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° from a median value of -138.0d. Finally, we find X-ray emission from the ``inner jet'' between 5" and 10" from the core.