Orbital eccentricity at 10 Hz (e_10 Hz) as a function of the coalescence time (t_coal) of BBH mergers in YSCs (left), GCs (centre), and NSCs (right). Different colours indicate mergers through flybys and the two families of exchanges. The yellow stars show second-generation BBH mergers. The empty black dots highlight the BBH progenitors of second-generation mergers. The dashed vertical line divides the plot into two regions: up to 1 Myr we evolve the systems with ARWV, above 1 Myr all the dynamical interactions are concluded, and with Eq. (1) we stop the ARWV integration and evolve the remaining BBHs. The three insets show a zoom for mergers with e_10 Hz > 0.1. We note that some of the points at e_10 Hz ∼ 1 overlap.