Application to three high-resolution cosmological re-simulations. First and second rows: face-on and edge-on density contours for the C1, C2, and C3 models. Third row: change in angular momentum as a function of disc radius: effective migration is seen for all models. Fourth row: vertical velocity dispersion profiles for non-migrators, outward and inward migrators. Fifth row: same but for the radial velocity dispersion. Bottom row: fractional contribution of migrators to the total vertical and radial velocity dispersions (as Fig. 6). Results are very similar to the simpler models presented earlier.