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Close, bright, and boxy: the superluminous SN 2018hti

https://doi.org/10.1093/mnras/stac744

Fiore, A. ; Benetti, S. ; Nicholl, M. ; Reguitti, A. ; Cappellaro, E. ; Campana, S. ; Bose, S. ; Paraskeva, E. ; Berger, E. ; Bravo, T. M. ; et al ( March 2022 , Monthly Notices of the Royal Astronomical Society)

ABSTRACT
SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of −21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ∼50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ∼10 M⊙ of circumstellar material or a magnetar with a magnetic field of Bp∼ 1.3 × 1013 G, and initial period of Pspin∼ 1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ${\sim}40\, \mathrm{M}_\odot$ progenitor star.

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