Notes. Minimal and maximal cumulative energy flow through the three r_s values for stellar populations of the considered metallicities and densities at the final time. Similarly, the minimal and maximal final kinetic energy fractions are shown. The values are IMF-weighted (normalised to the total mass in stars above 8 M_⊙), and a rotation distribution for single and orbital period distribution for binary stars, and a binary fraction is assumed. As comparison, the SN-only energy (without PION) for a population, if all single models in this work would undergo a CCSN with the canonical energy of 10⁵¹ erg would be 5.0 × 10⁴⁹ erg ${\mathrm{M}}_{\odot }^{-1}$, while considering the whole grid (with binary stars) in the same way would give 3.1 × 10⁴⁹ erg ${\mathrm{M}}_{\odot }^{-1}$ (see Sect. 2.2).