Figure 9

Final fates of Population III stars in the absence of stellar rotation. Above \({\simeq}30\mbox { M}_{\odot}\), a fraction of the star may collapse to a BH, while at higher masses it collapses directly to a BH or explodes as a pair-instability SN. The chemical yields of the ejecta depend sensitively on the fate of the star. The mass limits change if rotation is taken into account. Adapted from Heger and Woosley (2002).