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High-resolution observations of ionized and molecular gas in the nuclearregions of galaxies are indispensable for delineating the interplay of starformation, gaseous inflows, stellar radiation, and feedback processes.Combining our new ALMA band 3 mapping and archival VLT/MUSE data, we present aspatially resolved analysis of molecular and ionized gas in the central 5.4 Kpcregion of NGC 1365. We find the star formation rate/efficiency (SFR/SFE) in theinner 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-Schmidtlaw, demonstrating a steeper slope (1.96$\pm$0.14) than previous resultspresumably based on lower-resolution observations. Compared to the northeasterncounterpart, the southwestern dust lane shows lower SFE, but denser moleculargas, and larger virial parameters. This is consistent with an interpretation ofnegative feedback from AGN and/or starburst, in the sense that theradiation/winds can heat and interact with the molecular gas even in relativelydense regions. After subtracting the circular motion component of the moleculargas and the stellar rotation, we detect two prominent non-circular motioncomponents of molecular and ionized hydrogen gas, reaching a line-of-sightvelocity of up to 100 km/s. We conclude that the winds or shocked gas from thecentral AGN may expel the low-density molecular gas and diffuse ionized gas onthe surface of the rotating disk.

The Nuclear Region of NGC1365: Star Formation, Negative Feedback, and Outflow Structure