Column density along the z-axis (left panels) and along the y-axis (right panels) for the run with no feedback, NF1, (upper panels) and the run with scheme D (lower panels). Comparison with Fig. 1 clearly shows the drastic impact of the feedback. In particular, the run NF1 shows thin and long filaments in which self-gravitating fragments develop, indicating that the gas is primarily organised by self-gravity and undergoes run away collapse. The galactic disc is considerably thinner than when supernovae are included. On the other hand, run D shows a broader galactic disc than in runs C1 and C2, illustrating the importance of the spatial correlation between supernovae explosions and dense gas.