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Fig. 28.

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Observed late-time bolometric light curve (solid blue lines) and the fraction of light that could be attributed to 56Ni after accounting for CSM interaction (dashed, red). The dotted green curves show the 56Ni light curve after adding the missing IR flux (up to 5 μm). The IR correction pushes the light curves back to the regime of PISN models that produce 25–44 M of 56Ni. Even in the case of a substantial contribution from CSM interaction, a total amount of 25–44 M of 56Ni appears to be essential to power SN 2018ibb.

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