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Deriving circular velocities of galaxies from stellar kinematics can providean estimate of their total dynamical mass, provided a contribution from thevelocity dispersion of the stars is taken into account. Molecular gas (e.g.,CO) on the other hand, is a dynamically cold tracer and hence acts as anindependent circular velocity estimate without needing such a correction. Inthis paper we test the underlying assumptions of three commonly used dynamicalmodels, deriving circular velocities from stellar kinematics of 54 galaxies(S0-Sd) that have observations of both stellar kinematics from the CALIFAsurvey, and CO kinematics from the EDGE survey. We test the Asymmetric DriftCorrection (ADC) method, as well as Jeans, and Schwarzschild models. The threemethods each reproduce the CO circular velocity at 1Re to within 10%. All threemethods show larger scatter (up to 20%) in the inner regions (R < 0.4Re) whichmay be due to an increasingly spherical mass distribution (which is notcaptured by the thin disk assumption in ADC), or non-constant stellar M/Lratios (for both the JAM and Schwarzschild models). This homogeneous analysisof stellar and gaseous kinematics validates that all three models can recoverMdyn at 1Re to better than 20%, but users should be mindful of scatter in theinner regions where some assumptions may break down.

The EDGE-CALIFA survey: validating stellar dynamical mass models with CO kinematics