iPTF15dtg: a double-peaked Type Ic Supernova from a massive progenitor

TL;DR

This paper reports the discovery and analysis of iPTF15dtg, the first spectroscopically-normal double-peaked Type Ic supernova, revealing a massive progenitor star with an extended envelope through detailed observational and modeling efforts.

Contribution

It provides the first detailed study of a double-peaked Type Ic supernova, identifying the progenitor as a massive WR star with an extended envelope, and models the early emission with hydrodynamical simulations.

Findings

iPTF15dtg is a slow-rising, double-peaked Type Ic supernova.

The progenitor was a massive ($a0$35 M$_{a0}$) WR star with an extended low-mass envelope.

Hydrodynamical models reproduce the early emission with an extended ($a0$500 R$_{a0}$) envelope.

Abstract

Type Ic supernovae (SNe Ic) arise from the core-collapse of H (and He) poor stars, which could be either single WR stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak ($\sim$10-15 d), without any early (first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D). We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long ($\sim$30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic observed. We aim to determine the properties of this explosion and of its progenitor star. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modelled with hydrodynamical and analytical models, with particular focus on the early emission. Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modelling of the bolometric properties reveals a large ejecta mass ($\sim$10 $M_{\odot}$) and strong $^{56}$Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended ($\sim$500 R$_{\odot}$), low-mass ($\sim$0.045 M$_{\odot}$) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored. The large ejecta mass and the presence of H and He free extended material around the star suggest that the progenitor of iPTF15dtg was a massive ($\gtrsim$ 35 M$_{\odot}$) WR star suffering strong mass loss.