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

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 H I 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.