Cumulative distribution plot showing the number of hot stripped stars formed with mass greater than or equal to a given mass for all 100 runs at each metallicity. Lower metallicity environments form fewer high-mass stripped stars because of late expansion, but the expected total number of stripped stars is similar when considering a lower mass limit of ∼3 M_⊙ or lower. The different metallicity runs are marked with different colors, while we display the predictions for solar metallicity from Yungelson et al. (2024) using a dotted gray line.