  The inner-most region of the Seyfert galaxy NGC 2992 has long been suspected
to be the location of intense AGN-host galaxy interaction, but photon pile-up
in previous high-resolution observations hampered the study of soft X-ray
excess and the interaction near its nucleus. We present an X-ray imaging
spectroscopic analysis of the circumnuclear
($1^{\prime\prime}$--$3^{\prime\prime}$) region of NGC 2992 using the
zeroth-order image of a 135 ks grating observation obtained with Chandra, which
captured the nucleus in a historically low flux state. Extended soft X-ray
emission is detected in the circumnuclear region with observed luminosity
$L_{\rm X} \sim 7 \times 10^{39}\rm\ erg\ s^{-1}$. The majority of previously
puzzling detection of soft excess could be associated with the outflow,
indicated by the morphological correspondences between soft X-ray emission and
figure-eight-shaped radio bubbles. An anomalous narrow emission line with the
centroid energy $\sim4.97$ keV is found. If attributed to redshifted highly
ionized iron emission (e.g., Fe xxv), the required outflow velocity is
$\sim0.23\,c$. An alternative explanation is that this line emission could be
produced by the nuclear spallation of iron. We also find asymmetric extended Fe
K$\alpha$ emission along the galactic disk, which could originate from
reflection by cold gas on $\sim 200$ pc scale.
