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We have studied the X-ray emission within the inner 150 pc radius of NGC 4151by constructing high spatial resolution emission line images of OVII, OVIII,and NeIX. These maps show extended structures that are spatially correlatedwith the radio outflow and optical [OIII] emission. We find strong evidence forjet--gas cloud interaction, including morphological correspondences withregions of X-ray enhancement, peaks of near-infrared [FeII] emission, andoptical clouds. In these regions, moreover, we find evidence of elevatedNeIX/OVII ratios; the X-ray emission of these regions also exceeds thatexpected from nuclear photoionization. Spectral fitting reveals the presence ofa collisionally ionized component. The thermal energy of the hot gas suggeststhat >0.1% of the estimated jet power is deposited into the host interstellarmedium through interaction between the radio jet and the dense medium of thecircum-nuclear region. We find possible pressure equilibrium between thecollisionally ionized hot gas and the photoionized line-emitting cool clouds.We also obtain constraints on the extended iron and silicon fluorescentemission. Both lines are spatially unresolved. The upper limit on thecontribution of an extended emission region to the Fe Kalpha emission is <5% ofthe total, in disagreement with a previous claim that 65% of the Fe Kalphaemission originates in the extended narrow line region.

A Deep Chandra ACIS Study of NGC 4151. II. The Innermost Emission Line Region and Strong Evidence for Radio Jet-NLR Cloud Collision