Top: distribution of estimated ages of the cluster when the massive systems are ejected from the cluster, τ_ej, for three different (primary star) mass groups in the MS3UQ_SP model. All ejected systems from 100 runs for each model are counted. Bottom: averaged core radius, r_c, of the same model as a function of time (black line). The lower and upper boundary of the grey shaded area are the 17th and 84th percentile, i.e., 68% of clusters have a core radius ranging within the area. The secondary maximum is shown in the top panel near 2.1 Myr when the core radius shrinks again as a result of the Spitzer instability.