  We present a ~100 ksec Chandra X-ray observation and new VLA radio data of
the large scale, 300 kpc long X-ray jet in PKS1127-145, a radio loud quasar at
redshift z=1.18. With this deep X-ray observation we now clearly discern the
complex X-ray jet morphology and see substructure within the knots. The X-ray
and radio jet intensity profiles are seen to be strikingly different with the
radio emission peaking strongly at the two outer knots while the X-ray emission
is strongest in the inner jet region. The jet X-ray surface brightness
gradually decreases by an order of magnitude going out from the core. The new
X-ray data contain sufficient counts to do spectral analysis of the key jet
features. The X-ray energy index of the inner jet is relatively flat with
alpha_X = 0.66 +/-0.15 and steep in the outer jet with alpha_X = 1.0 +/-0.2. We
discuss the constraints implied by the new data on the X-ray emission models
and conclude that ``one-zone'' models fail and at least a two component model
is needed to explain the jet's broad-band emission. We propose that the X-ray
emission originates in the jet proper while the bulk of the radio emission
comes from a surrounding jet sheath. We also consider intermittent jet activity
as a possible cause of the observed jet morphology.
