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

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dc.contributor.authorFiore, A.
dc.contributor.authorBenetti, S.
dc.contributor.authorNicholl, M.
dc.contributor.authorReguitti, A.
dc.contributor.authorCappellaro, E.
dc.contributor.authorCampana, S.
dc.contributor.authorBose, S.
dc.contributor.authorParaskeva, E.
dc.contributor.authorBerger, E.
dc.contributor.authorBravo, T.M.
dc.contributor.authorBurke, J.
dc.contributor.authorCai, Y.-Z.
dc.contributor.authorChen, T.-W.
dc.contributor.authorChen, P.
dc.contributor.authorCiolfi, R.
dc.contributor.authorDong, S.
dc.contributor.authorGomez, S.
dc.contributor.authorGromadzki, M.
dc.contributor.authorGutiérrez, C.P.
dc.contributor.authorHiramatsu, D.
dc.contributor.authorHosseinzadeh, G.
dc.contributor.authorHowell, D.A.
dc.contributor.authorJerkstrand, A.
dc.contributor.authorKankare, E.
dc.contributor.authorKozyreva, A.
dc.contributor.authorMaguire, K.
dc.contributor.authorMcCully, C.
dc.contributor.authorOchner, P.
dc.contributor.authorPellegrino, C.
dc.contributor.authorPignata, G.
dc.contributor.authorPost, R.S.
dc.contributor.authorElias-Rosa, N.
dc.contributor.authorShahbandeh, M.
dc.contributor.authorSchuldt, S.
dc.contributor.authorThomas, B.P.
dc.contributor.authorTomasella, L.
dc.contributor.authorVinkó, J.
dc.contributor.authorVogl, C.
dc.contributor.authorWheeler, J.C.
dc.contributor.authorYoung, D.R.
dc.date.accessioned2024-05-24T15:59:08Z
dc.date.available2024-05-24T15:59:08Z
dc.date.issued2022-05-01
dc.descriptionIndexación: Scopus.
dc.description.abstractSN 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. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/512/3/4484/6549929
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Volume 512, Issue 3, Pages 4484 - 4502, 1 May 2022
dc.identifier.doi10.1093/mnras/stac744
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/57036
dc.language.isoen
dc.publisherOxford University Press
dc.rights.licensehttps://creativecommons.org/licenses/by/4.0/deed.es
dc.rights.uriCC BY 4.0 DEED Atribución 4.0 Internacional
dc.subjectSupernovae: general
dc.subjectSupernovae: individual: SN 2018hti
dc.subjectSupernovae
dc.subjectCircumstellar materials
dc.subjectLight curves
dc.subjectMagnetars
dc.subjectMagnetic-field
dc.subjectPhysical parameters
dc.subjectRisetimes
dc.subjectSpectra modeling
dc.subjectSupernovae: individual: sn 1987a
dc.titleClose, bright, and boxy: the superluminous SN 2018hti
dc.typeArtículo
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