Precision Determination of Corotation Radii in Galaxy Disks: Tremaine–Weinberg versus Font–Beckman for NGC 3433

Beckman, J. E.; Font, J.; Borlaff, A.; García-Lorenzo, B.
Bibliographical reference

The Astrophysical Journal, Volume 854, Issue 2, article id. 182, 7 pp. (2018).

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Density waves in galaxy disks have been proposed over the years, in a variety of specific models, to explain spiral arm structure and its relation to the mass distribution, notably in barred galaxies. An important parameter in dynamical density wave theories is the corotation radius, the galactocentric distance at which the stars and gas rotate at the same speed as the quasi-static propagating density wave. Determining corotation, and the pattern speed of a bar have become relevant to tests of cosmologically based theories of galaxy evolution involving the dynamical braking of bars by interaction with dark matter halos. Here, comparing two methods, one of that measures the pattern speed and another that measures the radius of corotation, using two instruments (an integral field spectrometer and a Fabry–Perot interferometer), and using both the stellar and interstellar velocity fields, we have determined the bar corotation radius, and three further radii of corotation for the SAB(s)b galaxy NGC 3433. The results of both methods, with both instruments, and with both disk components, give excellent agreement. This strengthens our confidence in the value of the two methods, and offers good perspectives for quantitative tests of different theoretical models.
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