Notes. Columns: (1) Model code: MmP[l/s][D/R][b/s], where m indicates the bulge-to-satellite mass ratio (m = 6, 9, or 18 for models with luminous mass ratios equal to 1:6, 1:9, 1:18, respectively), “Pl” refers to long pericentre and “Ps” to short pericentre, “D” indicates direct orbits and “R” retrograde orbits), and the final letter (“b” or “s”) indicates whether the primary galaxy had a large or a small bulge. The letter in parentheses helps us to identify each model quickly in the forthcoming figures; (2) model code in EM06, for those models that were already presented in that paper; (3) primary galaxy model used in the experiment (big or small primary bulge, see Table 1); (4) luminous mass ratio between satellite and primary galaxy; (5) ratio of the luminous half-mass radii of the satellite to the primary galaxy; (6) first pericentre distance of the orbit, in units of the primary disc scale-length; (7) initial angle between the orbital momentum and the primary disc spin. This angle determines whether the orbit is prograde (direct) or retrograde; (8) approximate time of full merger, in simulation units; (9) total run time of each experiment, in simulation units.