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

• Published in: Monthly notices of the Royal Astronomical Society Vol. 491; no. 2; p. 2902
• Main Authors: Flörs, A, Spyromilio, J, Taubenberger, S, Blondin, S, Cartier, R, Leibundgut, B, Dessart, L, Dhawan, S, Hillebrandt, W
• Format: Journal Article
• Language: English
• Published: Oxford University Press (OUP): Policy P - Oxford Open Option A 01.01.2020
• Subjects: line: formation; line: identification; radiation mechanisms: thermal; Sciences of the Universe; SN2017bzc; supernovae: general; supernovae: individual: SN2015F
• ISSN: 0035-8711; 1365-2966; 1365-2966
• DOI: 10.1093/mnras/stz3013

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 Å to 7 155 Å line as a prior in fits of spectra covering only the optical wavelengths we show that the 7200 Å 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 (MCh) and sub-Chandrasekhar mass (sub-MCh) 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-MCh explosion simulations of ∼Z⊙ progenitors. Only a small fraction (11%) of objects in the sample have a Ni/Fe abundance in agreement with MCh explosion models.