Tracks of a 20 M_⊙ star with initial rotation Ω/Ω_c = 0.6 and metallicity Z = 0.001, 0.0006, and 0.0003. The line styles and color code are the same as in Figure 1. We plot the tracks only until the end of C burning; afterward, in the very last stages of their evolution, the T_eff and luminosity oscillate widely in our MESA models, and we did not plot them in order to have a cleaner image (see, e.g., Costa et al. 2022). Even at these low metallicities, stars are able to activate thick winds and peel off their envelopes.