SDSS IV MaNGA: characterizing non-axisymmetric motions in galaxy velocity fields using the radon transform

David V. Stark, Kevin A. Bundy, Kyle Westfall, Matt Bershady, Anne-Marie Weijmans, Karen L. Masters, Sandor Kruk, Jarle Brinchmann, Juan Soler, Roberto Abraham, Edmond Cheung, Dmitry Bizyaev, Niv Drory, Alexandre Roman Lopes, David R. Law

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Abstract

We show how the Radon transform (defined as a series of line integrals through an image at different orientations and offsets from the origin) can be used as a simple, non-parametric tool to characterize galaxy velocity fields, specifically their global kinematic position angles (PA_k) and any radial variation or asymmetry in PA_k. This method is fast and easily automated, making it particularly beneficial in an era where IFU and interferometric surveys are yielding samples of thousands of galaxies. We demonstrate the Radon transform 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 and stellar velocity fields into five categories based on the shape of their radial PA_k profiles. At least half of stellar velocity fields and two-thirds of gas velocity fields are found to show detectable deviations from uniform coplanar circular motion, although most of these variations are symmetric about the center of the galaxy. The behavior of gas and stellar velocity fields is largely independent, even when PA_k profiles for both components are measured over the same radii. We present evidence that one class of symmetric PA_k variations is likely associated with bars and/or oval distortions, while another class is more consistent with warped disks. This analysis sets the stage for more in-depth future studies which explore the origin of diverse kinematic behavior in the galaxy population.
Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Early online date30 Jul 2018
DOIs
Publication statusEarly online - 30 Jul 2018

Keywords

  • astro-ph.GA
  • astro-ph.IM

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