Synthetic UV spectra for different metallicities Z from wind models for WNh stars from Gräfener & Hamann (2008). The presented models are computed for a luminosity of log (L/L_⊙) = 6.3, a stellar temperature T_⋆ = 44.7 kK, and have very similar mass-loss rates (~1.8 × 10^-5M_⊙ yr^-1). The given He ii line luminosities have only been determined for the narrow-emission components of the He ii line profiles. Measurement errors for the given L_{He ii}, FWHM, and EW probably amount to ~±0.05 dex (or ±10%).