Late-Time Hubble Space Telescope Observations of a Hydrogen-Poor Superluminous Supernova Reveal the Power-Law Decline of a Magnetar Central Engine

TL;DR

This study presents late-time Hubble observations of a hydrogen-poor superluminous supernova, revealing a magnetar-powered light curve decline that challenges the PISN hypothesis and suggests diverse energy sources.

Contribution

It demonstrates that late-time light curve analysis can distinguish between PISN and magnetar models in hydrogen-poor SLSNe, highlighting the role of magnetar spin-down.

Findings

Light curve flattening inconsistent with radioactive decay of $^{56}$Co.

Light curve matches magnetar spin-down with a shallower power law.

High ejecta mass (~20 M$_{ ext{odot}}$) inferred for the supernova.

Abstract

The light curve diversity of hydrogen-poor superluminous supernovae (SLSNe) has kept open the possibility that multiple power sources account for the population. Specifically, pair-instability explosions (PISNe), which produce large masses of $^{56}$Ni, have been argued as the origin of some slowly-evolving SLSNe. Here we present detailed observations of SN 2016inl (=PS16fgt), a slowly-evolving SLSN at $z=0.3057$, whose unusually red spectrum matches PS1-14bj, a SLSN with an exceptionally long rise time consistent with a PISN. Ground-based and Hubble Space Telescope data, spanning about 800 rest-frame days, reveal a significant light curve flattening, similar to that seen in SN 2015bn, and much slower than the decline rate expected from radioactive decay of $^{56}$Co. We therefore conclude that despite its slow evolution, SN 2016inl is inconsistent with a PISN. Instead, the light curve evolution matches the expected power-law spin-down of a magnetar central engine, but with a shallower power law ($L\propto t^{-2.8}$) compared to that in SN 2015bn, indicating a possible difference in the $\gamma$-ray opacity between the two events. Analytical modeling indicates typical magnetar engine parameters, but one of the highest ejecta masses ($\approx 20$ M$_{\odot}$) inferred for a SLSN. Our results indicate that monitoring the late-time light curve evolution of SLSNe provides a powerful diagnostic of their energy source.