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Fig. 1


a) Model of the spectrum of SN 2013cu at 15.5 h after the explosion (red-dashed line) and the respective observations from G14 (black). The strongest features are labeled. b) Example of a possible LBV pre-explosion spectrum of the progenitor of SN 2013cu. We note the huge difference in pre- and post-explosion morphology due to very different ionization conditions before and after the SN.

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