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

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 sy...

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Detalles Bibliográficos
Autores: Fiore, Achille, Benetti, Stefano, Nicholl, Matt, Reguitti, Andrea, Cappellaro, Enrico, Campana, Sergio, Bose, S., Paraskeva, E., Berger, E., Müller-Bravo, Tomás E., Burke, Jamison, Cai, Y-Z, Chen, T. W., Ciolfi, Riccardo, Dong, Subo, Gómez, Sergio, Gromadzki, Mariusz, Gutiérrez, Claudia P., Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. Andrew, Jerkstrand, Anders, Kankare, E., Kozyreva, A., Maguire, Kate, McCully, Curtis, Ochner, Paolo, Pellegrino, Conte, Pignata, Giuliano, Post, R. S., Elias-Rosa, Nancy, Shahbandeh, Melissa, Schuldt, S., Thomas, B. P., Tomasella, Lina, Vinkó, Jozsef, Vogl, Christian, Wheeler, J. Craig, Young, D. R.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/296536
Acceso en línea:http://hdl.handle.net/10261/296536
Access Level:acceso abierto
Palabra clave:Supernovae: general
Supernovae: individual: SN 2018hti
Descripción
Sumario: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.

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