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 ∼40M⊙ progenitor star.
Original language | English |
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Pages (from-to) | 4484-4502 |
Number of pages | 19 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 512 |
Issue number | 3 |
DOIs | |
State | Published - 1 May 2022 |
Keywords
- supernovae: general
- supernovae: individual: SN 2018hti