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Fig. 15


Comparison of optical spectra for a sample of observations and a selection of models presented in this work – we make no attempt at obtaining best fits. Apart from SN 2015bs, which stands apart, most of these well-observed SNe II show similar spectral properties at 300− 400 d after explosion. A variety of models is used to show the offsets caused by certain assumptions (for example, the weak [Ca II] λλ 7291, 7323 that follows from Ca over-ionization caused by strong 56Ni mixing in model m15mix100vnimH9). Model m15mix100mH9, used for SN 2012aw, would provide a better match to the observationsof SN 1999em.

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