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

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

doi:10.1093/mnras/stac744

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

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Kozyreva, A.
Stellar Astrophysics, MPI for Astrophysics, Max Planck Society;

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Schuldt, S.
Physical Cosmology, MPI for Astrophysics, Max Planck Society;

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Vogl, C.
Stellar Astrophysics, MPI for Astrophysics, Max Planck Society;

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Citation

Fiore, A., Benetti, S., Nicholl, M., Reguitti, A., Cappellaro, E., Campana, S., et al. (2022). Close, bright, and boxy: the superluminous SN 2018hti. Monthly Notices of the Royal Astronomical Society, 512(3), 4484-4502. doi:10.1093/mnras/stac744.

Cite as: https://hdl.handle.net/21.11116/0000-000B-530E-9

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 B_p∼ 1.3 × 10¹³ 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 ∼40M_⊙ progenitor star.