Illustration of the minimum initial mass required to appear as a WR star after stripping () and to reach the WR phase through intrinsic stripping (). Plotted are six BPASS evolution tracks at a fixed metallicity (0.008), three for single stars and three for binaries with an initial mass ratio of 0.9 and an initial period of P_i = 100 d. The initial mass of the single star or the primary is fixed to three distinct values, M_i <   ,   < M_i <  , and M_i >  . The dotted segments correspond to binary mass transfer phases. Only stars with M_i >   can undergo self-stripping. Stars with M_i <   can only be stripped in binaries, but only those with M_i >   will appear as WR stars after stripping. The insets represent possible normalized spectra of He stars found in the corresponding parameter regime, noting that significant deviations for individual objects are possible. Since the purpose of the figure is illustrative, the values of the initial masses and axis labels (which are model and Z-dependent) are omitted.