Ratio of the yields obtained in this work to those obtained by LC18, each weighted by a Salpeter IMF, averaged over the IDORV, and subsequently normalized to one. The red line shows the ratio of our yields to the original yields from LC18, for which every star explodes. The cyan line is the same as the red, except that we apply our explodability to the yields of LC18, analogously to what is done in Fig. 12. The empty circles and the dashed line connecting them indicate elements for which the total yield is less than 10⁻⁷ M_⊙. The very large discrepancies at low metallicities are due to the fact that these are typically higher-compactness stars and therefore are expected to eject high amounts of ⁵⁶Ni, which is, however, kept fixed at 0.07 M_⊙ in LC18 (see the text for more details).