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 which 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 \alpha = 0.60 \pm 0.05 ( where S _ { \nu } \propto \nu ^ { - \alpha } ) .
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 \alpha = 0.76 \pm 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 \times 10 ^ { 43 } erg/s ; substantially more power may be emitted in the 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 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 \pm 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 .