We apply the Tremaine–Weinberg method to 19 nearby galaxies using stellar mass surface densities and velocities derived from the PHANGS-MUSE survey, to calculate (primarily bar) pattern speeds (Ω_P). After quality checks, we find that around half (10) of these stellar-mass-based measurements are reliable. For those galaxies, we find good agreement between our results and previously published pattern speeds, and we use rotation curves to calculate major resonance locations (corotation radii and Lindblad resonances). We also compare these stellar-mass-derived pattern speeds with Hα (from MUSE) and CO(J = 2 − 1) emission from the PHANGS-ALMA survey. We find that in the case of these clumpy interstellar medium (ISM) tracers, this method erroneously gives a signal that is simply the angular frequency at a representative radius set by the distribution of these clumps (Ω_clump), and that this Ω_clump is significantly different from Ω_P (∼20% in the case of Hα, and ∼50% in the case of CO). Thus, we conclude that it is inadvisable to use “pattern speeds” derived from ISM kinematics. Finally, we compare our derived pattern speeds and corotation radii, along with bar properties, to the global parameters of these galaxies. Consistent with previous studies, we find that galaxies with a later Hubble type have a larger ratio of corotation radius to bar length, more molecular-gas-rich galaxies have higher Ω_P, and more bulge-dominated galaxies have lower Ω_P. Unlike earlier works, however, there are no clear trends between the bar strength and Ω_P, nor between the total stellar mass surface density and the pattern speed.

我们使用源自 PHANGS-MUSE 调查的恒星质量表面密度和速度将 Tremaine-Weinberg 方法应用于 19 个附近的星系，以计算（主要是条形）模式速度（Ω _P）。经过质量检查，我们发现这些基于恒星质量的测量中约有一半 (10) 是可靠的。对于这些星系，我们发现我们的结果与先前公布的模式速度之间有很好的一致性，我们使用旋转曲线来计算主要共振位置（共旋半径和 Lindblad 共振）。我们还将这些源自恒星质量的模式速度与 H α（来自 MUSE）和 CO（J= 2 − 1) PHANGS-ALMA 调查的排放量。我们发现，在这些团块星际介质 (ISM) 示踪剂的情况下，这种方法错误地给出了一个信号，该信号只是由这些团块的分布 (Ω _clump )设置的代表性半径处的角频率，并且这个 Ω_团块是与 Ω _P显着不同（H α的情况下约为 20%，在 CO 的情况下约为 50%）。因此，我们得出结论，不建议使用源自 ISM 运动学的“模式速度”。最后，我们将我们导出的模式速度和共转半径以及棒属性与这些星系的全局参数进行比较。与之前的研究一致，我们发现具有较晚哈勃类型的星系具有更大的共转半径与棒长的比率，更多富含分子气体的星系具有更高的Ω _P，而更多以膨胀为主的星系具有更低的Ω _P。然而，与早期的工作不同，棒强度和 Ω _P之间没有明显的趋势，总恒星质量表面密度和模式速度之间也没有明显的趋势。