Kinematic analysis of the super-extended HI disk of the nearby spiral galaxy M 83

Cosima Eibensteiner, Frank Bigiel, Adam K. Leroy, Eric W. Koch, Erik Rosolowsky, Eva Schinnerer, Amy Sardone, Sharon Meidt, W. J. G de Blok, David Thilker, D. J. Pisano, Jürgen Ott, Ashley Barnes, Miguel Querejeta, Eric Emsellem, Johannes Puschnig, Dyas Utomo, Ivana Bešlic, Jakob den Brok, Shahram FaridaniSimon C. O. Glover, Kathryn Grasha, Hamid Hassani, Jonathan D. Henshaw, Maria J. Jiménez-Donaire, Jürgen Kerp, Daniel A. Dale, J. M. Diederik Kruijssen, Sebastian Laudage, Patricia Sanchez-Blazquez, Rowan Smith, Sophia Stuber, Ismael Pessa, Elizabeth J. Watkins, Thomas G. Williams, Benjamin Winkel

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We present new HI observations of the nearby massive spiral galaxy M83, taken with the VLA at 21″ angular resolution (≈500 pc) of an extended (1.5 deg2) 10-point mosaic combined with GBT single dish data. We study the super-extended HI disk of M83 (∼50 kpc in radius), in particular disc kinematics, rotation and the turbulent nature of the atomic interstellar medium. We define distinct regions in the outer disk (rgal > central optical disk), including ring, southern area, and southern and northern arm. We examine HI gas surface density, velocity dispersion and non-circular motions in the outskirts, which we compare to the inner optical disk. We find an increase of velocity dispersion (σv) towards the pronounced HI ring, indicative of more turbulent HI gas. Additionally, we report over a large galactocentric radius range (until rgal ∼ 50 kpc) that σv is slightly larger than thermal (i.e. > 8 km s-1). We find that a higher star formation rate (as traced by FUV emission) is not always necessarily associated with a higher HI velocity dispersion, suggesting that radial transport could be a dominant driver for the enhanced velocity dispersion. We further find a possible branch that connects the extended HI disk to the dwarf irregular galaxy UGCA365, that deviates from the general direction of the northern arm. Lastly, we compare mass flow rate profiles (based on 2D and 3D tilted ring models) and find evidence for outflowing gas at rgal ∼ 2 kpc, inflowing gas at rgal ~ 5.5 kpc and outflowing gas at rgal ~ 14 kpc. We caution that mass flow rates are highly sensitive to the assumed kinematic disk parameters, in particular, to the inclination.
Original languageEnglish
Article numberA37
Number of pages24
JournalAstronomy & Astrophysics
Early online date29 Jun 2023
Publication statusPublished - Jul 2023


  • ISM: kinematics and dynamics
  • Radio lines: galaxies
  • Galaxies: groups: individual: M 83


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