Structure of the X-ray emission from the jet of 3C 273

We present images from five observations of the quasar 3C 273 with the Chan dra 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 v ery bright in X-rays. Its X-ray spectrum is well fitted with a power law wi th alpha = 0.60 +/- 0.05 (where S, proportional to nu (-alpha)). Combining this measurement with lower frequency data shows that a pure synchrotron mo del can fit the spectrum of this knot from 1.647 GHz to 5 keV (over nine de cades in energy) with alpha = 0.76 +/- 0.02, similar to the X-ray spectral slope. Thus, we place a lower limit on the total power radiated by this kno t of 1.5 x 10(43) ergs s(-1); substantially more power may be emitted in th e hard X-ray and gamma -ray bands. Knot A2 is also detected and is somewhat blended with knot B1. Synchrotron emission may also explain the X-ray emis sion, but a spectral bend is required near the optical band. For knots A1 a nd B1, the X-ray flux dominates the emitted energy. For the remaining optic al 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 excursio ns of +/- 1 degrees from a median value of -138.degrees0. Finally, we find X-ray emission from the "inner jet" between 5" and 10" from the core.