  Detection of hard X-ray spectrum (spectral index < 2) from the kilo-parsec
scale jet of active galactic nuclei cannot be accounted to the synchrotron
emission mechanism from the electron distribution responsible for the
radio/optical emission. Alternate explanations are the inverse Compton
scattering of cosmic microwave background photons (IC/CMB) or synchrotron
emission from a second electron population. When the X-ray emission is
interpreted as IC/CMB process, the Compton spectrum often peaks at GeV energy
and many sources were predicted to be the Fermi candidate sources. The absence
of significant gamma ray flux from some of these galaxies by Fermi disfavored
the IC/CMB interpretation of the high energy emission. We extend this study to
predict the very high energy (VHE) gamma ray emission due to IC/CMB model which
can be investigated by Cherenkov Telescope Array Observatory (CTAO). The model
parameters deciding the broadband spectral energy distribution are estimated
using analytical approximation of the emissivity functions. The emission model
is extrapolated to VHE energy and then compared with the CTAO sensitivity. For
this particular study, we have selected 18 knots with harder X-ray spectrum and
for which the IC/CMB model for X-ray emission was suggested.
