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

This is the authors' abstract. We don't add key points for this paper.

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.