  We use the results of relativistic hydrodynamic simulations of jet-ISM
interactions in a galaxy with a radio-loud AGN to quantify the extent of
ionization in the central few kpcs of the gaseous galactic disc. We perform
post-process radiative transfer of AGN radiation through the simulated gaseous
jet-perturbed disc to estimate the extent of photo-ionization by the AGN with
an incident luminosity of $10^{45}~\mathrm{erg\,s^{-1}}$. We also map the gas
that is collisionally ionized due to shocks driven by the jet. The analysis was
carried out for simulations with similar jet power
($10^{45}~\mathrm{erg\,s^{-1}}$) but different jet orientations with respect to
the gas disc. We find that the shocks from the jets can ionize a significant
fraction (up to 33$\%$) of dense gas ($n>100\,\mathrm{cm^{-3}}$) in the disc,
and that the jets clear out the central regions of gas for AGN radiation to
penetrate to larger distances in the disc. Jets inclined towards the disc plane
couple more strongly with the ISM and ionize a larger fraction of gas in the
disc as compared to the vertical jet. However, similar to previous studies, we
find that the AGN radiation is quickly absorbed by the outer layers of dense
clouds in the disc, and is not able to substantially ionize the disc on a
global scale. Thus, compared to jet-ISM interactions, we expect that
photo-ionization by the AGN radiation only weakly affects the star-formation
activity in the central regions of the galactic disc ($\lesssim 1$ kpc),
although the jet-induced shocks can spread farther out.
