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We model the gas dynamics of barred galaxies using a three-dimensional,high-resolution, $N$-body+hydrodynamical simulation and apply it to the MilkyWay in an attempt to reproduce both the large-scale structure and the clumpymorphology observed in Galactic H\emissiontype{I} and CO $l-v$ diagrams. Owingto including the multi-phase interstellar medium, self-gravity, star-formationand supernovae feedback, the clumpy morphology, as well as the large-scalefeatures, in observed $l-v$ diagrams are naturally reproduced. We identify inour $l-v$ diagrams with a number of not only large-scale peculiar features suchas the '3-kpc arm', '135-km s$^{-1}$ arm' and 'Connecting arm' but also clumpyfeatures such as `Bania clumps', and then link these features in a face-on viewof our model. We give suggestions on the real structure of the Milky Way and onthe fate of gas clumps in the central region.

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