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 ∼450 d after explosion. We detect the [Ni II] 1.939 µm 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 γ-ray observations, we find ∼0.05 M 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 ∼600 km s −1 .

Sub-Chandrasekhar progenitors favoured for type Ia supernovae: Evidence from late-time spectroscopy★.

“…The double peaked feature around 16 000 Å is composed of a blend of [Fe ii] and [Co ii] lines of the multiplets a 4 F-a 4 D and a 5 F-b 3 F, respectively. Redwards of the strong telluric absorption feature at ∼ 18 500 Å we also detect the a 2 F 7/2 -a 4 F 9/2 line of [Ni ii] in spectra with high SNR (Dhawan et al 2018).…”

Constraining Type Ia supernova asymmetry with the gamma-ray escape time-scale

“…Maeda et al (2010) use a 56 Ni zone going up to 12000 km s −1 in their toy model to fit nebular spectra. Mazzali et al (2015) find 56 Ni up to 8500 km s −1 in SN 2011fe, and Dhawan et al (2018) find 56 Ni up to 8600 km s −1 in SN 2014J. Black et al (2019) show evidence for iron clumps at velocities from 8500 to 12000 km s −1 .…”

Exploration of Aspherical Ejecta Properties in Type Ia Supernovae: Progenitor Dependence and Applications to Progenitor Classification

“…These techniques had been applied to a few well-observed SNe Ia, including SNe 2011fe, 2012cg, 2014J, and 2015F and SN remnant (SNR) 3C 397 (see recent work in, for example, Yamaguchi et al 2015;Dave et al 2017;Leung & Nomoto 2017aShen et al 2018;Zhou et al 2021). The progenitor mass and metallicity are constrained by this method, which allows further identification of isotopic mass fractions of radioactive Ni isotopes in SN 2012cg (Graur et al 2016) and SN 2014J (Yang et al 2018) and stable Ni by the nebular IR spectra (see Dhawan et al 2018, for the application to SN 2014J).…”

“…The closest SN Ia in the last four decades, SN 2014J is a special example of SNe Ia exploded in the nearby galaxy M82, just 3.3 Mpc away. Its closeness to the Milky Way has provided the chance for detailed multiband observations, including the radio (Pérez-Torres et al 2014), infrared, optical (Goobar et al 2014;Kawabata et al 2014), UV (Foley et al 2014), X-ray (Terada et al 2016), and gamma-ray (Diehl et al 2014;Churazov et al 2015;Diehl et al 2015;Diehl 2015;Isern et al 2016) bands, with its spectra at early and late times (Ashall et al 2014;Jack et al 2015;Dhawan et al 2018).…”

“…measurement is found inDiehl et al (2015), who gave  For 57 Ni,Yang et al (2018) reported that 57 Ni/ 56 Ni has a mass ratio of  0.065 0.004 0.005 based on the B-band maximum light and  0.066 0.008 0.009 based on the pseudobolometric light curve. Stable Ni mass is constrained at 0.053±0.018 M e(Dhawan et al 2018). …”