Astrophys. J., 549, L167-L171 (2001/March-2)
Structure of the X-ray emission from the jet of 3C 273.
MARSHALL H.L., HARRIS D.E., GRIMES J.P., DRAKE J.J., FRUSCIONE A., JUDA M., KRAFT R.P., MATHUR S., MURRAY S.S., OGLE P.M., PEASE D.O., SCHWARTZ D.A., SIEMIGINOWSKA A.L., VRTILEK S.D. and WARGELIN B.J.
Abstract (from CDS):
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 1.5x1043 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°.0. Finally, we find X-ray emission from the ``inner jet'' between 5" and 10" from the core.
Galaxies: Jets - Galaxies: Quasars: Individual: Alphanumeric: 3C 273 - X-Rays: Galaxies
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