Spectral energy distributions for stripped stars resulting from a 12 M_⊙ donor star for a range of different metallicities. These are modeled with CMFGEN assuming our standard wind mass loss rates. We indicate the ionization limits of hydrogen and helium with dotted lines. At high metallicity, the mass loss rates are higher, leading to a denser wind surrounding the star. Recombination in the wind of He²⁺ to He⁺ blocks the emission of photons with wavelengths shorter than λ = 228 Å for models with . The spectra of the metal-rich models show many characteristic emission lines. At lower metallicity, the winds are transparent and most lines are in absorption. The metal-poor stripped stars still have hydrogen at their surface. This is responsible for the characteristic drop at 912 Å. The stripped stars are also more luminous and somewhat cooler. All model spectra are created during core helium burning when central helium abundance is X_He,c = 0.5.