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.authorRosa N. E.
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.contributor.organizationfi=Suomen ESO-keskus|en=Finnish Centre for Astronomy with ESO|
dc.contributor.organizationfi=Tuorlan observatorio|en=Tuorla Observatory|
dc.contributor.organization-code1.2.246.10.2458963.20.54954054844
dc.contributor.organization-code1.2.246.10.2458963.20.90670098848
dc.converis.publication-id68078955
dc.converis.urlhttps://research.utu.fi/converis/portal/Publication/68078955
dc.date.accessioned2022-10-28T13:17:40Z
dc.date.available2022-10-28T13:17:40Z
dc.description.abstract<p>SN~2018hti was a very nearby (z=0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -22.2 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 days. 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 Msun of circumstellar material or a magnetar with a magnetic field of B_p~1.3e13 G and initial period of P_spin~1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ~40 Msun progenitor star.</p>
dc.format.pagerange4484
dc.format.pagerange4502
dc.identifier.eissn1365-2966
dc.identifier.jour-issn0035-8711
dc.identifier.olddbid181104
dc.identifier.oldhandle10024/164198
dc.identifier.urihttps://www.utupub.fi/handle/11111/54668
dc.identifier.urlhttps://academic.oup.com/mnras/article-abstract/512/3/4484/6549929
dc.identifier.urnURN:NBN:fi-fe2022081154537
dc.language.isoen
dc.okm.affiliatedauthorGutierrez, Claudia
dc.okm.affiliatedauthorKankare, Erkki
dc.okm.discipline115 Astronomy and space scienceen_GB
dc.okm.discipline115 Avaruustieteet ja tähtitiedefi_FI
dc.okm.internationalcopublicationinternational co-publication
dc.okm.internationalityInternational publication
dc.okm.typeA1 ScientificArticle
dc.publisher.countryUnited Kingdomen_GB
dc.publisher.countryBritanniafi_FI
dc.publisher.country-codeGB
dc.relation.doi10.1093/mnras/stac744
dc.relation.ispartofjournalMonthly Notices of the Royal Astronomical Society
dc.relation.issue3
dc.relation.volume512
dc.source.identifierhttps://www.utupub.fi/handle/10024/164198
dc.titleClose, bright and boxy: the superluminous SN 2018hti
dc.year.issued2022

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