  The relatively intense X-ray emission from large scale (tens to hundreds kpc)
jets discovered with Chandra likely implies that jets (at least in powerful
quasars) are still relativistic at that distances from the active nucleus. In
this case the emission is due to Compton scattering off seed photons provided
by the Cosmic Microwave Background, and this on one hand permits to have
magnetic fields close to equipartition with the emitting particles, and on the
other hand minimizes the requirements about the total power carried by the jet.
The emission comes from compact (kpc scale) knots, and we here investigate what
we can predict about the possible emission between the bright knots. This is
motivated by the fact that bulk relativistic motion makes Compton scattering
off the CMB photons efficient even when electrons are cold or mildly
relativistic in the comoving frame. This implies relatively long cooling times,
dominated by adiabatic losses. Therefore the relativistically moving plasma can
emit, by Compton scattering the microwave seed photons, for a long time. We
discuss how the existing radio--to--X-ray observations of large scale jets
already pose strong constraints on the structure and dynamics of knots and we
present a scenario that can satisfactorily reproduce the observed phenomenology
of the jet in 3C273. In this scenario the kiloparsec-scale knots visible with
HST, Chandra and VLA are composed of several smaller sub--units, accounting for
the fast decrease of the flux outside the large knot. Substructure in the
X-ray- emitting knots can also explain the month--year variability timescale
reported for the large scale jet in M87.
