SN 2016dsg: A Thermonuclear Explosion Involving A Thick Helium Shell

TL;DR

SN 2016dsg is a peculiar, sub-luminous Type I supernova likely caused by a thermonuclear explosion involving a thick helium shell on a white dwarf, showing unique spectral features and challenging existing models.

Contribution

This study presents detailed photometric and spectroscopic observations of SN 2016dsg, providing evidence for a helium-shell detonation on a white dwarf and highlighting discrepancies with current models.

Findings

Spectra show strong UV line blanketing and weak O I absorption.

Detection of helium in the near-infrared spectrum.

Photometric evolution not well matched by existing models.

Abstract

A thermonuclear explosion triggered by a helium-shell detonation on a carbon-oxygen white dwarf core has been predicted to have strong UV line blanketing at early times due to the iron-group elements produced during helium-shell burning. We present the photometric and spectroscopic observations of SN 2016dsg, a sub-luminous peculiar Type I SN consistent with a thermonuclear explosion involving a thick He shell. With a redshift of 0.04, the $i$-band peak absolute magnitude is derived to be around -17.5. The object is located far away from its host, an early-type galaxy, suggesting it originated from an old stellar population. The spectra collected after the peak are unusually red, show strong UV line blanketing and weak O I $\lambda$7773 absorption lines, and do not evolve significantly over 30 days. An absorption line around 9700-10500 \AA is detected in the near-infrared spectrum and is likely from the unburnt helium in the ejecta. The spectroscopic evolution is consistent with the thermonuclear explosion models for a sub-Chandrasekhar mass white dwarf with a thick helium shell, while the photometric evolution is not well described by existing models.