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We study the most luminous known supernova (SN) associated with a gamma-rayburst (GRB), SN 2011kl. The photospheric velocity of SN 2011kl around peakbrightness is $21,000\pm7,000$ km s$^{-1}$. Owing to different assumptionsrelated to the light-curve (LC) evolution (broken or unbroken power-lawfunction) of the optical afterglow of GRB 111209A, different techniques for theLC decomposition, and different methods (with or without a near-infraredcontribution), three groups derived three different bolometric LCs for SN2011kl. Previous studies have shown that the LCs without an early-time excesspreferred a magnetar model, a magnetar+$^{56}$Ni model, or a white dwarf tidaldisruption event model rather than the radioactive heating model. On the otherhand, the LC shows an early-time excess and dip that cannot be reproduced bythe aforementioned models, and hence the blue-supergiant model was proposed toexplain it. Here we reinvestigate the energy sources powering SN 2011kl. Wefind that the two LCs without the early-time excess of SN 2011kl can beexplained by the magnetar+$^{56}$Ni model, and the LC showing the early excesscan be explained by the magnetar+$^{56}$Ni model taking into account thecooling emission from the shock-heated envelope of the SN progenitor,demonstrating that this SN might primarily be powered by a nascent magnetar.

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