Kinematic analysis of the super-extended H I disk of the nearby spiral galaxy M 83^⋆,⋆⋆

¹ Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
e-mail: eibensteiner@astro.uni-bonn.de
² Department of Astronomy, The Ohio State University, 4055 McPherson Laboratory, 140 West 18th Ave, Columbus, OH, 43210 USA
³ Center for Astrophysics, Harvard & Smithsonian, 60 Garden St., 02138 Cambridge, MA, USA
⁴ Dept. of Physics, University of Alberta, Edmonton, Alberta, T6G 2E1 Canada
⁵ Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
⁶ Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium
⁷ Netherlands Institute for Radio Astronomy (ASTRON), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands
⁸ Kapteyn Astronomical Institute, University of Groningen, PO Box 800 9700 AV Groningen, The Netherlands
⁹ Department of Astronomy, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa
¹⁰ Department of Physics & Astronomy, Bloomberg Center for Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD, 21218 USA
¹¹ Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch, 7701 South Africa
¹² Department of Physics and Astronomy, West Virginia University, White Hall, Box 6315 Morgantown, WV, 26506 USA
¹³ Center for Gravitational Waves and Cosmology, West Virginia University, Chestnut Ridge Research Building, Morgantown, WV, 26505 USA
¹⁴ National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM, 87801 USA
¹⁵ European Southern Observatory, Karl-Schwarzschild Straße 2, 85748 Garching bei München, Germany
¹⁶ Observatorio Astronómico Nacional (IGN), C/ Alfonso XII, 3, 28014 Madrid, Spain
¹⁷ Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69230 Saint-Genis-Laval, France
¹⁸ National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA, 22903 USA
¹⁹ Institüt für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Strasse 2, 69120 Heidelberg, Germany
²⁰ Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT, 2611 Australia
²¹ Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool, L3 5RF UK
²² Department of Physics & Astronomy, University of Wyoming, Laramie, WY, 82071 USA
²³ Cosmic Origins Of Life (COOL) Research DAO, Munich, Germany
²⁴ Departamento de Fisica de la Tierra y Astrofisica & IPARCOS, Facultad de CC Fisicas, Universidad Complutense de Madrid, 28040 Madrid, Spain
²⁵ Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120 Heidelberg, Germany
²⁶ Sub-department of Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH UK
²⁷ Max-Planck-Institut für Radioastronomie, Radioobservatorium Effelsberg, Max-Planck-Strasse 28, Munich, Germany

Received: 24 October 2022
Accepted: 24 March 2023

Abstract

We present new H I observations of the nearby massive spiral galaxy M 83 taken with the JVLA at 21″ angular resolution (≈500 pc) of an extended (∼1.5 deg²) ten-point mosaic combined with GBT single-dish data. We study the super-extended H I disk of M 83 (∼50 kpc in radius), in particular disk kinematics, rotation, and the turbulent nature of the atomic interstellar medium. We define distinct regions in the outer disk (r_gal> central optical disk), including a ring, a southern area, a southern arm and a northern arm. We examine H I gas surface density, velocity dispersion, and noncircular motions in the outskirts, which we compare to the inner optical disk. We find an increase of velocity dispersion (σ_v) toward the pronounced H I ring, indicative of more turbulent H I gas. Additionally, we report over a large galactocentric radius range (until r_gal ∼ 50 kpc) where σ_v is slightly larger than thermal component (i.e., > 8 km s⁻¹). We find that a higher star-formation rate (as traced by far UV emission) is not necessarily always associated with a higher H I velocity dispersion, suggesting that radial transport could be a dominant driver for the enhanced velocity dispersion. Furthermore, we find a possible branch that connects the extended H I disk to the dwarf irregular galaxy UGCA 365 and 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 r_gal ∼ 2 kpc, inflowing gas at r_gal ∼ 5.5 kpc, and outflowing gas at r_gal ∼ 14 kpc. We caution that mass flow rates are highly sensitive to the assumed kinematic disk parameters, in particular to inclination.