2018ApJ...857...88J

We present Hubble Space Telescope observations and photometric measurements of the Type Ia supernova (SN Ia) SN 2013aa 1500 days after explosion. At this epoch, the luminosity is primarily dictated by the amounts of radioactive ⁵⁷Co and ⁵⁵Fe, while at earlier epochs, the luminosity depends on the amount of radioactive ⁵⁶Co. The ratio of odd-numbered to even-numbered isotopes depends significantly on the density of the progenitor white dwarf (WD) during the SN explosion, which, in turn, depends on the details of the progenitor system at the time of ignition. From a comprehensive analysis of the entire light curve of SN 2013aa, we measure a M(⁵⁷Co)/M(⁵⁶Co) ratio of 0.02_–0.02^+0.01, which indicates a relatively low central density for the progenitor WD at the time of explosion, consistent with DD progenitor channels. We estimate M(⁵⁶Ni)=0.732±0.151 M_☉, and place an upper limit on the abundance of ⁵⁵Fe. A recent study reported a possible correlation between M(⁵⁷Co)/M(⁵⁶Co) and stretch for four SNe Ia. SN 2013aa, however, does not fit this trend, indicating either SN 2013aa is an extreme outlier or the correlation does not hold up with a larger sample. The M(⁵⁷Co)/M(⁵⁶Co) measured for the expanded sample of SNe Ia with photometry at extremely late times has a much larger range than that of explosion models, perhaps limiting conclusions about SN Ia progenitors drawn from extremely late-time photometry.