Fig. A.3
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Initial-final-mass relation (IFMR): the BH mass mBH versus the progenitor ZAMS star mass mZAMS for all eight simulations. Columns from left to right show increasing rotation ω0 = 0.0, 0.6, 1.2, 1.8. K runs use a white background; NOK runs are shaded light grey. Blue lines separate the progenitor-mass regimes, as annotated in red. Orange lines enclose the pair-instability mass gap (∼64-161 M⊙, Woosley & Heger 2021). IMBHs appear below, within and above the PISN gap.
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