Close, bright and boxy: the superluminous SN 2018hti
Fiore A.; Reguitti A.; Howell D. A.; Ciolfi R.; Bose S.; Burke J.; Hiramatsu D.; Maguire K.; Tomasella L.; Young D. R.; Bravo T. M.; Vinkó J.; Pellegrino C.; McCully C.; Vogl C.; Campana S.; Pignata G.; Berger E.; Benetti S.; Jerkstrand A.; Gromadzki M.; Chen P.; Shahbandeh M.; Chen T.-W.; Paraskeva E.; Gomez S.; Thomas B. P.; Hosseinzadeh G.; Cappellaro E.; Ochner P.; Cai Y.-Z.; Gutiérrez C. P.; Kozyreva A.; Wheeler J. C.; Nicholl M.; Post R. S.; Kankare E.; Rosa N. E.; Schuldt S.; Dong S.
https://urn.fi/URN:NBN:fi-fe2022081154537
Tiivistelmä
SN~2018hti was a very nearby (z=0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -22.2 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 days. 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 Msun of circumstellar material or a magnetar with a magnetic field of B_p~1.3e13 G and initial period of P_spin~1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ~40 Msun progenitor star.
Kokoelmat
- Rinnakkaistallenteet [19207]