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

A. Fiore, S. Benetti, M. Nicholl, A. Reguitti, E. Cappellaro, S. Campana, S. Bose, E. Paraskeva, E. Berger, T. M. Bravo, J. Burke, Y. -Z. Cai, T. -W. Chen, P. Chen, R. Ciolfi, S. Dong, S. Gomez, M. Gromadzki, C. P. Gutiérrez, D. HiramatsuG. Hosseinzadeh, D. A. Howell, A. Jerkstrand, E. Kankare, A. Kozyreva, K. Maguire, C. McCully, P. Ochner, C. Pellegrino, G. Pignata, R. S. Post, N. Elias-Rosa, M. Shahbandeh, S. Schuldt, B. P. Thomas, L. Tomasella, J. Vinkó, C. Vogl, J. C. Wheeler, D. R. Young

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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 40 progenitor star.
Original languageEnglish
Pages (from-to)4484–4502
Number of pages19
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Early online date17 Mar 2022
Publication statusPublished - May 2022


  • supernovae: general
  • supernovae: individual: SN 2018hti


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