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Fig. 2.

image

CMFGEN optical spectra of SNe interacting with their progenitor’s wind at early times for solar (top panel), CNO-processed (middle panel), and He-rich abundances (bottom panel). 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. All the models in this figure have = 3 × 10−3 M yr−1. The labels indicate the adopted values of L9 (109L), and the strongest spectral lines are identified.

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