{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/applying-the-tremaine-weinberg-method-to","title":"Applying the Tremaine-Weinberg Method to Nearby Galaxies: Stellar Mass-Based Pattern Speeds, and Comparisons with ISM Kinematics","arxiv_id":"2102.01091","date":"2021-02-01","proceeding":null,"authors":["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"],"abstract":"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 ($\\Omega_{\\rm P}$). 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 H$\\alpha$ (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 ($\\Omega_{\\rm clump}$), and that this $\\Omega_{\\rm clump}$ is significantly different to $\\Omega_{\\rm P}$ ($\\sim$20% in the case of H$\\alpha$, and $\\sim$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 $\\Omega_{\\rm P}$, and more bulge-dominated galaxies have lower $\\Omega_{\\rm P}$. Unlike earlier works, however, there are no clear trends between the bar strength and $\\Omega_{\\rm P}$, nor between the total stellar mass surface density and the pattern speed.","url_abs":"https://arxiv.org/abs/2102.01091v2","url_pdf":"https://arxiv.org/pdf/2102.01091v2.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"applying-the-tremaine-weinberg-method-to","repo_url":"https://github.com/thomaswilliamsastro/phangs_pattern_speeds","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":0,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}