Details

Autor(en) / Beteiligte

• 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

Titel

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

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2022-04, Vol.512 (3), p.4484-4502

Ort / Verlag

Oxford University Press

Erscheinungsjahr

2022

Quelle

EZB Free E-Journals

Beschreibungen/Notizen

• 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.