Nebular spectroscopy of SN 2014J: Detection of stable nickel in near infrared spectra

Abstract

We present near infrared (NIR) spectroscopy of the nearby supernova 2014J obtained \(\sim\)450 d after explosion. We detect the [Ni II] 1.939 \(\mu\)m line in the spectra indicating the presence of stable \(^{58}\)Ni in the ejecta. The stable nickel is not centrally concentrated but rather distributed as the iron. The spectra are dominated by forbidden [Fe II] and [Co II] lines. We use lines, in the NIR spectra, arising from the same upper energy levels to place constraints on the extinction from host galaxy dust. We find that that our data are in agreement with the high \(A_V\) and low \(R_V\) found in earlier studies from data near maximum light. Using a \(^{56}\)Ni mass prior from near maximum light \(\gamma\)-ray observations, we find \(\sim\)0.05 M\(_\odot\) of stable nickel to be present in the ejecta. We find that the iron group features are redshifted from the host galaxy rest frame by \(\sim\)600 km s\(^{-1}\).