  We present the results of the spatial and spectral analysis of the deep (~200
ksec) Chandra HETG observation of the changing look AGN NGC7582. During this
observation NGC7582 was in a highly obscured state. Therefore, we considered
also a short Suzaku observation, which caught NGC7582 in a Compton thick state.
This allows us to determine the underlying continuum and the amount of
absorption ($N_H \sim~1.2\times10^{24}$ cm$^{-2}$). A wealth of emission lines
are detected in the Chandra data, which allow us to map the structure of the
circum-nuclear emitters. The high resolution spectrum reveals that the soft
X-ray emission originates in a hybrid gas, which is ionized in part by the
starforming activity and in part by the central AGN. The high resolution images
confirm that the emitting region is inhomogeneous and extends up to a few
hundred pc from the nuclear source. The X-ray images are more extended in the
lower energy lines (Ne and Mg) than in the higher energy lines (Si, Fe), where
the former are dominated by the collisionally ionised gas and the latter by the
photoionized AGN emission. This is supported by the analysis of the He-like
triplets. We deduce that a low density photoionized gas is responsible for the
strong forbidden components, which is likely to originate from extended AGN
Narrow Line Region gas at distances of 200-300 pc from the black hole. We also
detected an absorption feature at ~ 6.7 keV consistent with the rest frame
energy of the resonance absorption line from FeXXV, which traces the presence
of a sub-parsec scale ionized absorber. The emerging picture is in agreement
with our view of the circumnuclear gas in AGN, where the medium is clumpy and
stratified in both density and ionization. These absorbers and emitters are
located on different scales: from the sub-pc Broad Line Region gas out to the
kpc scale of the galactic absorber.
