Applying the Tremaine-Weinberg Method to Nearby Galaxies: Stellar-mass-based Pattern Speeds and Comparisons with ISM Kinematics

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00553757" target="_blank" >RIV/67985815:_____/21:00553757 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.3847/1538-3881/abe243" target="_blank" >https://doi.org/10.3847/1538-3881/abe243</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-3881/abe243" target="_blank" >10.3847/1538-3881/abe243</a>

Result language

angličtina

Original language name

Applying the Tremaine-Weinberg Method to Nearby Galaxies: Stellar-mass-based Pattern Speeds and Comparisons with ISM Kinematics

Original language description

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(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 H alpha (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 (omega(clump)), and that this omega(clump) is significantly different from omega(P) (similar to 20% in the case of H alpha, and similar to 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 omega(P), and more bulge-dominated galaxies have lower omega(P). Unlike earlier works, however, there are no clear trends between the bar strength and omega(P), nor between the total stellar mass surface density and the pattern speed.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

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Continuities

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Publication year

2021

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomical Journal

ISSN

0004-6256

e-ISSN

1538-3881

Volume of the periodical

161

Issue of the periodical within the volume

4

Country of publishing house

US - UNITED STATES

Number of pages

21

Pages from-to

185

UT code for WoS article

000629140700001

EID of the result in the Scopus database

2-s2.0-85103492933