Fig. 8.
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Comparison between supernova models and the observed r-band optical light curve. The best-fits to the second component are shown for a range of MOSFiT models (default, magnetar, magni, csm, and csmni; see Section 4.6.1). Fits to the other filters (z and J) are either poor, or require large amounts of dust and extreme absolute magnitudes.
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