  We present a deep Chandra spectral and spatial study of the kpc-scale diffuse
X-ray emission of the Compton thick (CT) AGN ESO428-G014. The entire spectrum
is best fit with composite photoionization + thermal models. The diffuse
emission is more extended at the lower energies (<3 keV). The smaller extent of
the hard continuum and Fe K{\alpha} profiles imply that the optically thicker
clouds responsible for this scattering may be relatively more prevalent closer
to the nucleus. These clouds must not prevent soft ionizing X-rays from the AGN
escaping to larger radii, in order to have photoionized ISM at larger radii.
This suggests that at smaller radii there may be a larger population of
molecular clouds to scatter the hard X-rays, as in the Milky Way. The diffuse
emission is also significantly extended in the cross-cone direction, where the
AGN emission would be mostly obscured by the torus in the standard AGN model.
Our results suggest that the transmission of the obscuring region in the
cross-cone direction is ~10% than in the cone-direction. In the 0.3-1.5 keV
band, the ratio of cross-cone to cone photons increases to ~84\%, suggesting an
additional soft diffuse emission component, disjoint from the AGN. This could
be due to hot ISM trapped in the potential of the galaxy. The luminosity of
this component ~5 10^38 erg s^-1 is roughly consistent with the thermal
component suggested by the spectral fits in the 170-900 pc annulus.
