CMFGEN optical spectra of SNe interacting with their progenitor’s wind at early times for progenitors with υ_∞ = 150 km s⁻¹ (models from Fig. 1; black) and with υ_∞ = 15 km s⁻¹ (overplotted on the corresponding high υ_∞ models; yellow). The models have been convolved with a Gaussian kernel of Δv = 300 km s⁻¹ (resolving power R ≈ 1000), continuum normalised, and shifted for clarity. The labels indicate the adopted values of Ṁ₃ (10⁻³ M_⊙ yr⁻¹), and the strongest spectral lines are identified. All the models in this figure have solar abundances and L = 1.5 × 10⁹ L_⊙.