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

研究成果: 雜誌貢獻期刊論文同行評審

5 引文 斯高帕斯(Scopus)


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 ∼40M⊙ progenitor star.

頁(從 - 到)4484-4502
期刊Monthly Notices of the Royal Astronomical Society
出版狀態已出版 - 1 5月 2022


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