Modeling The Most Luminous Supernova Associated with a Gamma-Ray Burst, SN 2011kl

Abstract

We study the most luminous known supernova (SN) associated with a gamma-ray burst (GRB), SN 2011kl. The photospheric velocity of SN 2011kl around peak brightness is $21,000\pm 7,000$ km s${}^{-1}$. Owing to different assumptions related to the light-curve (LC) evolution (broken or unbroken power-law function) of the optical afterglow of GRB 111209A, different techniques for the LC decomposition, and different methods (with or without a near-infrared contribution), three groups derived three different bolometric LCs for SN 2011kl. Previous studies have shown that the LCs without an early-time excess preferred a magnetar model, a magnetar+${}^{56}$Ni model, or a white dwarf tidal disruption event model rather than the radioactive heating model. On the other hand, the LC shows an early-time excess and dip that cannot be reproduced by the aforementioned models, and hence the blue-supergiant model was proposed to explain it. Here we reinvestigate the energy sources powering SN 2011kl. We find that the two LCs without the early-time excess of SN 2011kl can be explained by the magnetar+${}^{56}$Ni model, and the LC showing the early excess can be explained by the magnetar+${}^{56}$Ni model taking into account the cooling emission from the shock-heated envelope of the SN progenitor, demonstrating that this SN might primarily be powered by a nascent magnetar.

arXiv comment11 pages, 3 figures, 1 table, accepted for publication in ApJ

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Cited by in corpus (9)

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• A fallback accretion model for the unusual type II-P supernova iPTF14hls
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• Exploring GRBs and supernovae connection: does a superluminous hypernova population exist?
• Modeling the Light Curves of the Luminous Type Ic Supernova 2007D