Binding energy distribution for stars and COs in all simulated clusters at |$t=10$| Myr (top) and |$t=100$| Myr (bottom). Once the systems contain at least one MBH (middle and left panels) objects can become unbound (positive energies). In particular at early times (⁠|$t=10 \,\,\mathrm{ Myr}$|⁠, middle panel) the high-energy objects can be clearly seen. At later times many of the early escapers have travelled beyond 100 pc and have been removed from the simulation. There is no clear trend with the shape of the cluster merger orbit or the merging process itself.