Abstract:
Black-hole-driven outflows in galaxies hosting active galactic nuclei (AGN) may interact with their interstellar
medium (ISM) affecting star formation (SF). Such feedback processes, reminiscent of those seen in massive
galaxies, have been reported recently in some dwarf galaxies. However, such studies have usually been on
kiloparsec and larger scales and our knowledge of the smallest spatial scales to which these feedback processes can
operate is unclear. Here we demonstrate radio jet−ISM interaction on the scale of an asymmetric triple radio
structure of ∼10 pc size in NGC 4395. This triple radio structure is seen in the 15 GHz continuum image and the
two asymmetric jet-like structures are situated on either side of the radio core that coincides with the optical Gaia
position. The high-resolution radio image and the extended [O III]λ5007 emission, indicative of an outflow, are
spatially coincident and are consistent with the interpretation of a low-power radio jet interacting with the ISM.
Modelling of the spectral lines using MAPPINGS, and estimation of temperature using optical integral field
spectroscopic data suggest shock ionization of the gas. The continuum emission at 237 GHz, though weak, was
found to spatially coincide with the AGN. However, the CO(2−1) line emission was found to be displaced by
around 20 pc northward of the AGN core. The spatial coincidence of molecular H2λ2.4085 along the jet direction,
the morphology of ionized [O III]λ5007, and displacement of the CO(2−1) emission argues for conditions less
favorable for SF in the central ∼10 pc region.
