  The beamed inverse Compton/cosmic microwave background model has generally
been used for the interpretation of X-ray radiation from kiloparsec-scale jets
of the core-dominated quasars. Recent \textit{Fermi}-LAT and \textit{HST}
observations have brought this model into question. We examine the assumption
that X-rays from the kiloparsec-scale jet of the quasar PKS~1127$-$145 are
produced by inverse Compton scattering of the central source emission. In this
context, we show that both similarity and distinction between the observed
radio and X-ray spectral indices for some of the jet knots can be explained
under a single power-law electron energy distribution. We derive that the
viewing angle of the kiloparsec-scale jet is about $35^\circ$ and the jet has a
moderate relativistic speed of $\approx 0.8c$. The predicted gamma-ray flux of
the jet is found to be a few orders of magnitude lower than the minimum flux
level measured by \textit{Fermi}-LAT, further supporting our scenario.
