  Imaging X-ray spectroscopy of nearby AGNs, mostly with Chandra, has shown
that extended soft (<2.5 keV) emission-line dominated X-ray biconical
structures, of kiloparsec scale, are widespread in highly absorbed Compton
Thick (CT) AGNs. The X-ray emission is complex, requiring both photoionized and
shock-ionized gas. It originates from high ionization regions and is surrounded
by cocoons of low ionization narrow line emission regions (LINERS). Bicone 3-6
keV continuum and 6.4 keV Fe Kalpha emission has been detected, contrary to the
standard AGN model expectation that would confine this hard emission to the
pc-size nuclear absorbing torus. Extended emission in the cross-cone direction,
also requires modifications to the AGN standard model. A porous torus, with a
significant fraction of escaping AGN continuum, and/or jet interaction with ISM
creating a blow-back towards the nuclear region seem to be required. Here we
discuss these results and their implications for both the AGN model and our
understanding of AGN feedback. The finding of hot and highly photoionized gas
on 10s parsecs to several kiloparsec scales demonstrates that all three
feedback mechanisms are at work: radiation affects the inner molecular clouds
of the host on a ~1 kpc scale; shocks of relativistic jets with the host ISM a
few kpc from the central AGN; and photoionization of the ISM via winds on
scales from pc to multiple kpc. These results demonstrate that X-rays are
needed to develop a complete picture of AGN/host interaction along with radio
continuum, mm and sub-mm molecular line emission, and optical/near-IR emission
lines.
