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Fig. 9


Similar to Fig. 3, but now showing the influence of the progenitor H-rich envelope mass on the synthetic optical and near-infrared spectra at 300 d. The models shown are m25mix100vni and m25mix100vnimH9 (strong mixing of 56Ni but weak mixing of other species) and correspond to a 25 M progenitor star. There is a greater fraction of the total decay power absorbed in the H-rich layers of the lighter model m25mix100vni, boosting the [Ca II] λλ 7291, 7323 doublet emission, but this has an adverse effect on Hα, which pushes its formation to the outer lower density regions. These differences reflect in part the different distribution of decay-power absorbed since the two ejecta have a different velocity structure – mixing should also differ in nature for ejecta with a similar kinetic energy but a different mass (e.g., as in SNe II and Ibc).

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