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

TL;DR

This study uses spectral modeling of Type Ia supernovae to determine Ni/Fe abundance ratios, providing evidence that most originate from sub-Chandrasekhar mass explosions, challenging traditional models.

Contribution

It introduces a spectral analysis method to distinguish between Chandrasekhar and sub-Chandrasekhar mass progenitors in SNe Ia.

Findings

85% of normal SNe Ia have Ni/Fe ratios consistent with sub-Chandrasekhar models.

Only 11% of SNe Ia match Chandrasekhar mass explosion predictions.

Spectral modeling effectively differentiates progenitor mass in supernovae.

Abstract

A non-local-thermodynamic-equilibrium (NLTE) level population model of the first and second ionisation stages of iron, nickel and cobalt is used to fit a sample of XShooter optical + near-infrared (NIR) spectra of Type Ia supernovae (SNe Ia). From the ratio of the NIR lines to the optical lines limits can be placed on the temperature and density of the emission region. We find a similar evolution of these parameters across our sample. Using the evolution of the Fe II 12$\,$570$\,\mathring{A}\,$to 7$\,$155$\,\mathring{A}\,$line as a prior in fits of spectra covering only the optical wavelengths we show that the 7200$\,\mathring{A}\,$feature is fully explained by [Fe II] and [Ni II] alone. This approach allows us to determine the abundance of Ni II$\,$/$\,$Fe II for a large sample of 130 optical spectra of 58 SNe Ia with uncertainties small enough to distinguish between Chandrasekhar mass (M$_{\text{Ch}}$) and sub-Chandrasekhar mass (sub-M$_{\text{Ch}}$) explosion models. We conclude that the majority (85$\%$) of normal SNe Ia have a Ni/Fe abundance that is in agreement with predictions of sub-M$_{\text{Ch}}$ explosion simulations of $\sim Z_\odot$ progenitors. Only a small fraction (11$\%$) of objects in the sample have a Ni/Fe abundance in agreement with M$_{\text{Ch}}$ explosion models.