Open Access

Fig. 21

image

Same as Fig. 16, but now for the comparison between model s25A (M(56Ni) = 0.157M; left) and s25p2 (M(56Ni) = 0.112M; right) and observations of SN 2015bs (M(56Ni) = 0.048M). Both models adopt a solar metallicity, not exactly consistent with the one tenth solar metallicity inferred for SN 2015bs (Anderson et al. 2018). The flux normalization is done at the Hα rest wavelength in both panels. Some gaussian smoothing has been applied to the observed spectrum to reduce the level of noise.

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