  We present the first results from an X-ray and optical survey of a sample of
AGN radio jets with Chandra and HST. We focus here on the first six sources
observed at X-rays, in four of which a bright X-ray jet was detected for the
first time. In three out of four cases optical emission from the jet is also
detected in our HST images. We compare the X-ray morphology with the radio as
derived from improved processing of archival VLA data and we construct spectral
energy distributions (SED) for the most conspicuous emission knots. In most
cases the SEDs, together with the similarity of the X-ray and radio
morphologies, favor an inverse Compton origin of the X-rays. The most likely
origin of the seed photons is the Cosmic Microwave Background, implying the
jets are still relativistic on kiloparsec scales. However, in the first knot of
the PKS 1136-135 jet, X-rays are likely produced via the synchrotron process.
In all four cases bulk Lorentz factors of a few are required. The radio maps of
the two jets not detected by either Chandra or HST suggest that they are less
beamed at large scales than the other four detected sources. Our results
demonstrate that, at the sensitivity and resolution of Chandra, X-ray emission
from extragalactic jets is common, yielding essential information on their
physical properties.
