Plots regarding the amplitude of the Ƨ shape (a–b), average mass along the tail (c), and kinematics of the tail (d–f). (a) r_{galactocentric} histogram for the M20000, M4641 and M1000 models at an age of 500 Myr. The leading (solid lines) and trailing (dashed lines) are shown separately. (b) The distribution of distance_along_orbit with r_{galactocentric} for the same models in (a). The central 2R_tidal region is omitted while plotting the distributions in (a) and (b). (c) Average stellar mass as a function of distance_along_orbit in 200 pc bins for the models M20000, M4641 and M1000 (at an age of 1000 Myr). The shaded regions indicate 5-95 percentile values of the stellar masses. The dashed lines show the average mass of all stars in each simulation. (d–f) The variation in distance_along_orbit with v_{galactocentric} (d) total specific energy (e) and the time since escape (f) for M20000, M4641, and M1778 for their oldest snapshot. The dashed orange lines in panel f represent stars moving with a speed of 1.5 pc Myr⁻¹ (= 1.47 km s⁻¹) away from the cluster. Similar plots for M20000_e are given in Fig A.4.