Structure of the X-ray Emission from the Jet of 3C 273

Details Structure of the X-ray Emission from the Jet of 3C 273 Structure of the X-ray Emission from the Jet of 3C 273

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000head....5.0505m&link_type=abstract

American Astronomical Society, HEAD Meeting #5, #05.05; Bulletin of the American Astronomical Society, Vol. 32, p.1190

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We present images from several observations of the quasar 3C 273 with the Chandra X-ray Observatory. The zeroth order images from two grating observations using the ACIS-S detector and two others from direct imaging observations are used to determine spectrum of the jet and these are combined with an HRC-I image to obtain a broad-band X-ray image. The jet has at several distinct features which were 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 = 0.86 +/- 0.11. Combining this measurement with lower frequency data shows that a pure synchrotron model can fit the spectrum of this knot from 4 GHz to 5 keV (over nine decades in energy) with α = 0.82 +/- 0.01, consistent with the X-ray spectral slope. Thus, we can only place a lower limit on the total power radiated by this knot of 7 x 1043 erg/s; more power may be emitted in the γ -ray band. Knot A2 is also detected and is somewhat blended with knot B1; again, synchrotron emission may explain the X-ray emission. For these two knots, the X-ray flux dominates the emitted energy. This work was funded in part by contract SAO SV1-61010 and NASA contract NAS8-39073.

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