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

Abstract

We model the gas dynamics of barred galaxies using a three-dimensional, high-resolution, $N$-body+hydrodynamical simulation and apply it to the Milky Way in an attempt to reproduce both the large-scale structure and the clumpy morphology observed in Galactic H\emissiontype{I} and CO $l-v$ diagrams. Owing to including 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 are naturally reproduced. We identify 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 link 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.

accepted to PASJ

References in corpus (6)

• Molecular Hydrogen and Global Star Formation Relations in Galaxies
• Gas flow models in the Milky Way embedded bars
• 3D Distribution of Molecular Gas in the Barred Milky Way
• The origin of large peculiar motions of star-forming regions and spiral structures of our Galaxy
• The Effect of the Interstellar Model on Star Formation Properties in Galactic Disks
• Errors in kinematic distances and our image of the Milky Way Galaxy

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