Close, bright, and boxy: the superluminous SN 2018hti
Date Issued
2022
Author(s)
Fiore, A.
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Nicholl, M.
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Reguitti, A.
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Bose, S.
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Paraskeva, E.
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Berger, E.
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Bravo, T. M.
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Burke, J.
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Cai, Y. -Z.
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Chen, T. -W.
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Chen, P.
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Dong, S.
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Gomez, S.
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Gromadzki, M.
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Gutiérrez, C. P.
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Hiramatsu, D.
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Hosseinzadeh, G.
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Howell, D. A.
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Jerkstrand, A.
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Kankare, E.
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Kozyreva, A.
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Maguire, K.
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McCully, C.
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Ochner, P.
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Pellegrino, C.
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Pignata, G.
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Post, R. S.
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Shahbandeh, M.
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Schuldt, S.
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Thomas, B. P.
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Vinkó, J.
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Vogl, C.
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Wheeler, J. C.
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Young, D. R.
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.
Volume
512
Issue
3
Start page
4484
Issn Identifier
0035-8711
Ads BibCode
2022MNRAS.512.4484F
Rights
open.access
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