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The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less $^{56}$Ni ($\\lesssim 0.06\\ M_{\\odot}$) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. 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Miller, Alexei V. Filippenko, Avishay Gal-Yam, Kelsey I. Clubb, Nathan Smith, Ori D. Fox, Patrick L. Kelly, Ryan J. Foley, Sagi Ben-Ami, S. Bradley Cenko, Schuyler D. Van Dyk, Weikang Zheng, William H. Lee","submitted_at":"2013-12-13T23:40:11Z","abstract_excerpt":"We have obtained early-time photometry and spectroscopy of Supernova (SN) 2013df in NGC 4414. The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less $^{56}$Ni ($\\lesssim 0.06\\ M_{\\odot}$) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. 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