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Fig. 25.

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Comparison of SN 2018ibb with the PISN models P250Ni25 and P250Ni34 from Kozyreva et al. (2017; left panel) and the He100, He125, and He130 from Heger & Woosley (2002; right panel). Templates with nickel masses of 34–44 M are required to describe the entire bolometric light curve from tmax–93 to tmax+706 days. Models with M(Ni)=25 M systematically underestimate the observed bolometric light curve, but they could still be viable if CSM interaction contributes significantly throughout the evolution.

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