Extreme Supernova Models for the Superluminous Transient ASASSN-15lh

TL;DR

This paper models the superluminous transient ASASSN-15lh as a powerful core-collapse supernova interacting with a hydrogen-poor shell, with possible additional magnetar energy input, to explain its extreme luminosity and spectral features.

Contribution

It introduces a hybrid supernova model combining ejecta-CSM interaction and magnetar energy to explain ASASSN-15lh's luminosity, favoring a single-input interaction scenario.

Findings

Best fit with a ~40 Msun progenitor and ~20 Msun hydrogen-poor shell

Magnetar contribution can enhance luminosity but requires fine-tuning

Ejecta-CSM interaction explains late-time UV-bright plateau

Abstract

The recent discovery of the unprecedentedly superluminous transient ASASSN-15lh (or SN 2015L) with its UV-bright secondary peak challenges all the power-input models that have been proposed for superluminous supernovae. Here we examine some of the few viable interpretations of ASASSN-15lh in the context of a stellar explosion, involving combinations of one or more power inputs. We model the lightcurve of ASASSN-15lh with a hybrid model that includes contributions from magnetar spin-down energy and hydrogen-poor circumstellar interaction. We also investigate models of pure circumstellar interaction with a massive hydrogen-deficient shell and discuss the lack of interaction features in the observed spectra. We find that, as a supernova ASASSN-15lh can be best modeled by the energetic core-collapse of a ~40 Msun star interacting with a hydrogen-poor shell of ~20 Msun. The circumstellar shell and progenitor mass are consistent with a rapidly rotating pulsational pair-instability supernova progenitor as required for strong interaction following the final supernova explosion. Additional energy injection by a magnetar with initial period of 1-2 ms and magnetic field of 0.1-1 x 10^14 G may supply the excess luminosity required to overcome the deficit in single-component models, but this requires more fine-tuning and extreme parameters for the magnetar, as well as the assumption of efficient conversion of magnetar energy into radiation. We thus favor a single-input model where the reverse shock formed in a strong SN ejecta-CSM interaction following a very powerful core-collapse SN explosion can supply the luminosity needed to reproduce the late-time UV-bright plateau.