Near-infrared Spectral Evolution of the Type Ia Supernova 2014J in the Nebular Phase: Implications for the Progenitor System

As the closest Type Ia supernova in decades, SN 2014J provides a unique opportunity for detailed investigation into observational signatures of the progenitor system, explosion mechanism, and burning product distribution. We present a late-time near-infrared spectral series from Gemini-N at 307-466 days after the explosion. Following the H-band evolution probes the distribution of radioactive iron group elements, the extent of mixing, and the presence of magnetic fields in the expanding ejecta. Comparing the isolated 1.6440 μm [Fe II] emission line with synthetic models shows consistency with a Chandrasekhar mass white dwarf of 0.7 10 g cm c r = 9^-3 undergoing a delayed detonation The ratio of the flux in the neighboring 1.54 mm emission feature to the flux in the 1.6440 mm feature shows evidence of some limited mixing of stable and radioactive iron group elements in the central regions. Additionally, the evolution of the 1.6440 mm line shows an intriguing asymmetry. When measuring line width of this feature, the data show an increase in line width not seen in the evolution of the synthetic spectra, corresponding to ≈1000 km s-1, which could be caused by a localized transition to detonation producing asymmetric ionization in the ejecta. Using the difference in width between the different epochs, an asymmetric component in the central regions, corresponding to approximately the inner 2×10^-4 of white dwarf mass suggests an off-center ignition of the initial explosion and hence of the kinematic center from the chemical center. Several additional models investigated, including a He detonation and a merger, have difficulty reproducing the features seen in these spectra.