The detonation of a sub-Chandrasekhar-mass white dwarf at the origin of the low-luminosity Type Ia supernova 1999by

TL;DR

This study demonstrates that a sub-Chandrasekhar-mass white dwarf detonation model better explains the observed properties of low-luminosity Type Ia supernova 1999by than traditional Chandrasekhar-mass models, highlighting the importance of progenitor mass.

Contribution

It introduces a detailed sub-Chandrasekhar-mass white dwarf detonation model that matches observations of SN 1999by, providing evidence for progenitors below the Chandrasekhar limit.

Findings

Sub-Chandrasekhar model has shorter rise time and higher peak luminosity.

Model reproduces observed colors and decline rates of SN 1999by.

Absence of [Ni II] lines supports low stable nickel in the ejecta.

Abstract

While Chandrasekhar-mass ($M_{\rm Ch}$) models with a low $^{56}\rm{Ni}$ yield can match the peak luminosities of fast-declining, 91bg-like Type Ia supernovae (SNe Ia), they systematically fail to reproduce their faster light-curve evolution. Here we illustrate the impact of a low ejecta mass on the radiative display of low-luminosity SNe Ia, by comparing a sub-$M_{\rm Ch}$ model resulting from the pure central detonation of a C-O White Dwarf (WD) to a $M_{\rm Ch}$ delayed-detonation model with the same $^{56}\rm{Ni}$ yield of 0.12 M$_{\odot}$. Our sub-$M_{\rm Ch}$ model from a 0.90 M$_{\odot}$ WD progenitor has a $\sim$5 day shorter rise time in the integrated UV-optical-IR (uvoir) luminosity, as well as in the $B$-band, and a $\sim$20 per cent higher peak uvoir luminosity ($\sim$1 mag brighter peak $M_B$). This sub-$M_{\rm Ch}$ model also displays bluer maximum-light colours due to the larger specific heating rate, and larger post-maximum uvoir and $B$-band decline rates. The luminosity decline at nebular times is also more pronounced, reflecting the enhanced escape of gamma rays resulting from the lower density of the progenitor WD. The deficit of stable nickel in the innermost ejecta leads to a notable absence of forbidden lines of [Ni II] in the nebular spectra. In contrast, the $M_{\rm Ch}$ model displays a strong line due to [Ni II] 1.939 $\mu\rm{m}$, which could in principle serve to distinguish between different progenitor scenarios. Our sub-$M_{\rm Ch}$ model offers an unprecedented agreement with optical and near-infrared observations of the 91bg-like SN 1999by, making a strong case for a WD progenitor significantly below the Chandrasekhar-mass limit for this event and other low-luminosity SNe Ia.