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Applying the Tremaine-Weinberg Method to Nearby Galaxies: Stellar Mass-Based Pattern Speeds, and Comparisons with ISM Kinematics
Thomas G. Williams, Eva Schinnerer, Eric Emsellem, Sharon Meidt, Miguel Querejeta, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Mélanie Chevance, Daniel A. Dale, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, J. M. Diederik Kruijssen, Adam K. Leroy, Hsi-An Pan, Jérôme Pety, Ismael Pessa, Erik Rosolowsky, Toshiki Saito, Francesco Santoro, Andreas Schruba, Mattia C. Sormani, Jiayi Sun, Elizabeth J. Watkins
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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 use rotation curves to calculate major resonance locations (co-rotation 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 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 to 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 co-rotation 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 co-rotation 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.
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