2016ApJ...819...31G

Seitenzahl et al. have predicted that roughly three years after its explosion, the light we receive from a Type Ia supernova (SN Ia) will come mostly from reprocessing of electrons and X-rays emitted by the radioactive decay chain ⁵⁷Co - ⁵⁷Fe, instead of positrons from the decay chain ⁵⁶Co - ⁵⁶Fe that dominates the SN light at earlier times. Using the Hubble Space Telescope, we followed the light curve of the SN Ia SN 2012cg out to 1055 days after maximum light. Our measurements are consistent with the light curves predicted by the contribution of energy from the reprocessing of electrons and X-rays emitted by the decay of ⁵⁷Co, offering evidence that ⁵⁷Co is produced in SN Ia explosions. However, the data are also consistent with a light echo ∼14 mag fainter than SN 2012cg at peak. Assuming no light-echo contamination, the mass ratio of ⁵⁷Ni and ⁵⁶Ni produced by the explosion, a strong constraint on any SN Ia explosion models, is 0.043_–0.011^+0.012, roughly twice Solar. In the context of current explosion models, this value favors a progenitor white dwarf with a mass near the Chandrasekhar limit.