The Nuclear Region of NGC1365: Star Formation, Negative Feedback, and
  Outflow Structure
  High-resolution observations of ionized and molecular gas in the nuclear
regions of galaxies are indispensable for delineating the interplay of star
formation, gaseous inflows, stellar radiation, and feedback processes.
Combining our new ALMA band 3 mapping and archival VLT/MUSE data, we present a
spatially resolved analysis of molecular and ionized gas in the central 5.4 Kpc
region of NGC 1365. We find the star formation rate/efficiency (SFR/SFE) in the
inner circumnuclear ring is about 0.4/1.1 dex higher than in the outer regions.
At a linear resolution of 180 pc, we obtain a super-linear Kennicutt-Schmidt
law, demonstrating a steeper slope (1.96$\pm$0.14) than previous results
presumably based on lower-resolution observations. Compared to the northeastern
counterpart, the southwestern dust lane shows lower SFE, but denser molecular
gas, and larger virial parameters. This is consistent with an interpretation of
negative feedback from AGN and/or starburst, in the sense that the
radiation/winds can heat and interact with the molecular gas even in relatively
dense regions. After subtracting the circular motion component of the molecular
gas and the stellar rotation, we detect two prominent non-circular motion
components of molecular and ionized hydrogen gas, reaching a line-of-sight
velocity of up to 100 km/s. We conclude that the winds or shocked gas from the
central AGN may expel the low-density molecular gas and diffuse ionized gas on
the surface of the rotating disk.
