Simulating nearby disc galaxies on the main star formation sequence : II. The gas structure transition in low and high stellar mass discs
Recent hydrodynamical simulations of isolated barred disc galaxies have suggested a structural change in the distribution of the interstellar medium (ISM) around a stellar mass M∗ of 1010 M⊙. In the higher-mass regime (M∗ ≤ 1010 M⊙), we observe the formation of a central gas and stellar disc with a typical size of a few hundred parsecs connected through lanes to the ends of the stellar bar. In the
