  We report the results of joint Chandra/ACIS - NuSTAR deep observations of NGC
1167, the host galaxy of the young radio jet B2 0258+35. In the ACIS data we
detect X-ray emission, extended both along and orthogonal to the jet. At the
end of the SE radio jet, we find lower-energy X-ray emission that coincides
with a region of CO turbulence and fast outflow motions. This suggests that the
hot Interstellar Medium (ISM) may be compressed by the jet and molecular
outflow, resulting in more efficient cooling. Hydrodynamic simulations of
jet-ISM interaction tailored to NGC 1167 are in agreement with this conclusion
and with the overall morphology and spectra of the X-ray emission. The faint
hard nuclear source detected with Chandra and the stringent NuSTAR upper limits
on the harder X-ray emission show that the active galactic nucleus (AGN) in NGC
1167 is in a very low-accretion state. However, the characteristics of the
extended X-ray emission are more consonant to those of luminous Compton Thick
AGNs, suggesting that we may be observing the remnants of a past high accretion
rate episode, with sustained strong activity lasting ~ 2 x 103 yr. We conclude
that NGC1167 is presently a LINER, but was an AGN in the past, given the
properties of the extended X-ray emission and their similarity with those of CT
AGN extended emission.
