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 Atacama Large Millimeter/submillimeter Array band 3 mapping and archival Very Large Telescope/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 superlinear Kennicutt–Schmidt law, demonstrating a steeper slope (1.96 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 an active galactic nucleus (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 noncircular motion components of molecular and ionized hydrogen gas, reaching a line-of-sight velocity of up to 100 km s⁻¹. 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.

对星系核区电离和分子气体的高分辨率观测对于描绘恒星形成、气体流入、恒星辐射和反馈过程的相互作用是必不可少的。结合我们新的阿塔卡马大毫米/亚毫米阵列波段 3 测绘和超大望远镜/MUSE 档案数据，我们对 NGC 1365 中央 5.4 kpc 区域的分子和电离气体进行了空间解析分析。我们发现了恒星形成率/效率(SFR/SFE) 在内部环核中比外部区域高约 0.4/1.1 dex。在 180 pc 的线性分辨率下，我们获得了超线性 Kennicutt-Schmidt 定律，表明比以前基于较低分辨率观测的结果更陡峭的斜率 (1.96 0.14)。与东北同行相比，西南尘埃带的 SFE 较低，但分子气体密度较大，维里参数较大。这与对来自活动星系核 (AGN) 和/或星暴的负反馈的解释一致，因为即使在相对密集的区域，辐射/风也可以加热并与分子气体相互作用。在减去分子气体的圆周运动分量和恒星自转后，我们检测到分子气体和电离氢气的两个突出的非圆周运动分量，视线速度可达 100 km s 从某种意义上说，即使在相对密集的区域，辐射/风也可以加热并与分子气体相互作用。在减去分子气体的圆周运动分量和恒星自转后，我们检测到分子气体和电离氢气的两个突出的非圆周运动分量，视线速度可达 100 km s 从某种意义上说，即使在相对密集的区域，辐射/风也可以加热并与分子气体相互作用。在减去分子气体的圆周运动分量和恒星自转后，我们检测到分子气体和电离氢气的两个突出的非圆周运动分量，视线速度可达 100 km s^-1。我们得出结论，来自中央AGN的风或冲击气体可能会在旋转盘表面驱逐低密度分子气体和扩散电离气体。