Eibensteiner, C.Bigiel, F.Leroy, A. K.Koch, E. W.Rosolowsky, E.Schinnerer, E.Sardone, A.Meidt, S.Sánchez Blázquez, PatriciaWinkel, B.2026-05-202026-05-202023Eibensteiner, C., Bigiel, F., Leroy, A. K., Koch, E. W., Rosolowsky, E., Schinnerer, E., ... & Winkel, B. (2023). Kinematic analysis of the super-extended H I disk of the nearby spiral galaxy M 83. Astronomy & Astrophysics, 675, A37.0004-636110.1051/0004-6361/202245290https://hdl.handle.net/20.500.14352/136793©The authors 2023 Artículo firmado por 36 autoresWe 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 deg^(2)) 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 rgal ∼ 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.engAttribution 4.0 Internationalhttp://creativecommons.org/licenses/by/4.0/journal article1432-0746https://doi.org/10.1051/0004-6361/202245290https://www.aanda.org/articles/aa/full_html/2023/07/aa45290-22/aa45290-22.htmlopen access5252-33ISM: kinematics and dynamicsRadio lines: galaxiesGalaxies: groupsGalaxies: individualGalaxies: M83Astrofísica21 Astronomía y Astrofísica