The dimensionless spin of resulting BHs for our W-R star models if their masses and angular momenta at the end of helium burning are preserved. Zahn’s predictions for the same system are also shown, and are assumed 1 (maximum rotating) if the progenitors have J > GM ²/c. For short initial orbits, the models typically predict higher spins than individual stellar evolution models, where the spins could be as low as 10⁻². However, the spins are usually lower than Zahn’s predictions, especially for high-mass systems.