Time sequence of the stellar surface density distribution of a typical star cluster merger simulations with an orbital eccentricity |$\mathrm{e}=0.05$| and an MBH in each cluster centre. We show the simulation at an early interacting phase (left panel, t = 0.5 Myr), at the time of the merger of the cluster cores (middle panel, t = 1 Myr), and after the central MBHs have formed a hard binary in the centre of the merger remnant (right panel, t = 15 Myr). By interactions with the MBH binary stars (star, white arrows), stellar BHs (BH, orange arrow), and WDs (WD, cyan arrow) can be ejected at high velocities after interacting with the MBH binary (a few examples are shown). The arrow length scales with velocity and the BH has a velocity of |$v_{\mathrm{ej}} \approx 80 \mathrm{~km} \mathrm{~s}^{-1}$|⁠.