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ABSTRACT  We present an analysis of Space Telescope Imaging Spectrograph (STIS)/ Hubble Space Telescope  optical spectra of a sample of 10 Seyfert galaxies aimed at studying the structure and physical properties of the coronal‐line region (CLR). The high spatial resolution provided by STIS allowed us to resolve the CLR and obtain key information about the kinematics of the CL gas, measure directly its spatial scale, and study the mechanisms that drive the high‐ionization lines. We find CLRs extending from just a few parsecs ( pc) up to 230 pc in radius, consistent with the bulk of the coronal lines (CLs) originating between the broad‐line region and narrow‐line region (NLR), and extending into the NLR in the case of [Fe  vii ] and [Ne  v ] lines. The CL profiles strongly vary with the distance to the nucleus. We observed line splitting in the core of some of the galaxies. Line peak shifts, both redshift and blueshift, typically reached 500 km s −1 , and even higher velocities (1000 km s −1 ) in some of the galaxies. In general, CLs follow the same pattern of rotation curves as low‐ionization lines like [O  iii ]. From a direct comparison between the radio and the CL emission we find that neither the strength nor the kinematics of the CLs scales in any obvious and strong way with the radio jets. Moreover, the similarity of the flux distributions and kinematics of the CLs and low‐ionization lines, the low temperatures derived for the gas, and the success of photoionization models to reproduce, within a factor of a few, the observed line ratios, point towards photoionization as the main driving mechanism of CLs.

Demystifying the coronal‐line region of active galactic nuclei: spatially resolved spectroscopy with the Hubble Space Telescope