On the Interpretation of the l–v Features in the Milky Way Galaxy

• Published in: Publications of the Astronomical Society of Japan Vol. 62; no. 6; pp. 1413 - 1422
• Main Authors: Junichi, Baba, Takayuki, R. Saitoh, Keiichi, Wada
• Format: Journal Article
• Language: English
• Published: Oxford, UK Oxford University Press 25-12-2010
• Subjects: Galaxy: disk; methods: numerical; Galaxy: kinematics and dynamics; galaxies: spiral; galaxies: ISM
• ISSN: 0004-6264; 2053-051X
• DOI: 10.1093/pasj/62.6.1413

We modeled the gas dynamics of barred galaxies using a three-dimensional, high-resolution,
$N$
-body
$+$
hydrodynamical simulation, and applied it to the Milky Way in an attempt to reproduce both the large-scale structure and the clumpy morphology observed in galactic HI and CO
$l$
–
$v$
diagrams. Owing to including of the multi-phase interstellar medium, self-gravity, star-formation, and supernovae feedback, the clumpy morphology, as well as the large-scale features, in observed
$l$
–
$v$
diagrams were naturally reproduced. We identified in our
$l$
–
$v$
diagrams with a number of not only large-scale peculiar features, such as the `3-kpc arm', `135-km s
$^{-1}$
arm', and `Connecting arm', but also clumpy features, such as `Bania clumps', and then linked these features in a face-on view of our model. We give suggestions on the real structure of the Milky Way and on the fate of gas clumps in the central region.