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We show how the Radon transform (defined as a series of line integralsthrough an image at different orientations and offsets from the origin) can beused as a simple, non-parametric tool to characterize galaxy velocity fields,specifically their global kinematic position angles (PA_k) and any radialvariation or asymmetry in PA_k. This method is fast and easily automated,making it particularly beneficial in an era where IFU and interferometricsurveys are yielding samples of thousands of galaxies. We demonstrate the Radontransform by applying it to gas and stellar velocity fields from the first~2800 galaxies of the SDSS-IV MaNGA IFU survey. We separately classify gas andstellar velocity fields into five categories based on the shape of their radialPA_k profiles. At least half of stellar velocity fields and two-thirds of gasvelocity fields are found to show detectable deviations from uniform coplanarcircular motion, although most of these variations are symmetric about thecenter of the galaxy. The behavior of gas and stellar velocity fields islargely independent, even when PA_k profiles for both components are measuredover the same radii. We present evidence that one class of symmetric PA_kvariations is likely associated with bars and/or oval distortions, whileanother class is more consistent with warped disks. This analysis sets thestage for more in-depth future studies which explore the origin of diversekinematic behavior in the galaxy population.

SDSS IV MaNGA: Characterizing Non-Axisymmetric Motions in Galaxy Velocity Fields Using the Radon Transform