SIMBAD references

2022MNRAS.512.4484F - Mon. Not. R. Astron. Soc., 512, 4484-4502 (2022/May-3)

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., MULLER BRAVO T., BURKE J., CAI Y.-Z., CHEN T.-W., CHEN P., CIOLFI R., DONG S., GOMEZ S., GROMADZKI M., GUTIERREZ 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., VINKO J., VOGL C., WHEELER J.C. and YOUNG D.R.

Abstract (from CDS):

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 x 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 ∼40 M☉ progenitor star.

Abstract Copyright: © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society

Journal keyword(s): supernovae: general - supernovae: individual: SN 2018hti

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 24

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