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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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.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/296536
Acesso em linha:http://hdl.handle.net/10261/296536
Access Level:acceso abierto
Palavra-chave:Supernovae: general
Supernovae: individual: SN 2018hti
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network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv Close, bright, and boxy: the superluminous SN 2018hti
title Close, bright, and boxy: the superluminous SN 2018hti
spellingShingle Close, bright, and boxy: the superluminous SN 2018hti
Fiore, Achille
Supernovae: general
Supernovae: individual: SN 2018hti
title_short Close, bright, and boxy: the superluminous SN 2018hti
title_full Close, bright, and boxy: the superluminous SN 2018hti
title_fullStr Close, bright, and boxy: the superluminous SN 2018hti
title_full_unstemmed Close, bright, and boxy: the superluminous SN 2018hti
title_sort Close, bright, and boxy: the superluminous SN 2018hti
dc.creator.none.fl_str_mv 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.
author Fiore, Achille
author_facet 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.
author_role author
author2 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.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv European Commission
University of Hawaii
Ministero dell'Istruzione, dell'Università e della Ricerca
Comisión Nacional de Investigación Científica y Tecnológica (Chile)
Fondo Nacional de Desarrollo Científico y Tecnológico (Chile)
European Research Council
Agencia Nacional de Investigación y Desarrollo (Chile)
National Science Foundation (US)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Supernovae: general
Supernovae: individual: SN 2018hti
topic Supernovae: general
Supernovae: individual: SN 2018hti
description 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.
publishDate 2022
dc.date.none.fl_str_mv 2022
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/296536
url http://hdl.handle.net/10261/296536
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/H2020/101004719
info:eu-repo/grantAgreement/EC/H2020/842471
info:eu-repo/grantAgreement/EC/H2020/758638
Monthly Notices of the Royal Astronomical Society
The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stac744
https://doi.org/10.1093/mnras/stac744
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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spelling Close, bright, and boxy: the superluminous SN 2018htiFiore, AchilleBenetti, StefanoNicholl, MattReguitti, AndreaCappellaro, EnricoCampana, SergioBose, S.Paraskeva, E.Berger, E.Müller-Bravo, Tomás E.Burke, JamisonCai, Y-ZChen, T. W.Ciolfi, RiccardoDong, SuboGómez, SergioGromadzki, MariuszGutiérrez, Claudia P.Hiramatsu, DaichiHosseinzadeh, GriffinHowell, D. AndrewJerkstrand, AndersKankare, E.Kozyreva, A.Maguire, KateMcCully, CurtisOchner, PaoloPellegrino, ContePignata, GiulianoPost, R. S.Elias-Rosa, NancyShahbandeh, MelissaSchuldt, S.Thomas, B. P.Tomasella, LinaVinkó, JozsefVogl, ChristianWheeler, J. CraigYoung, D. R.Supernovae: generalSupernovae: individual: SN 2018htiSN 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.MG is supported by the EU Horizon 2020 research and innovation programme under grant agreement No 101004719. MS acknowledges the Infrared Telescope Facility, which is operated by the University of Hawaii under contract 80HQTR19D0030 with the National Aeronautics and Space Administration. NER acknowledges support from MIUR, PRIN 2017 (grant 20179ZF5KS). TMB was funded by the CONICYT PFCHA / DOCTORADOBECAS CHILE/2017-72180113. AJ acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 Research and Innovation Program (ERC Starting Grant. AR acknowledges support from ANID BECAS/DOCTORADO NACIONAL 21202412. Y-Z Cai is funded by China Postdoctoral Science Foundation (grant no. 2021M691821). T-WC acknowledges the EU Funding under Marie Skłodowska-Curie grant H2020-MSCA-IF-2018-842471. KM is funded by the EU H2020 ERC grant no. 758638. GP is supported by ANID - Millennium Science Initiative - ICN12_009. We thank the staff at the different observatories for performing the observations. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects). ePESSTO+ observations were obtained under ESO program id 199.D-0143 (PI: Inserra). Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. This work uses observations from the Las Cumbres Observatory network. The LCO team is supported by NSF grants AST-1911225 and AST-1911151.Peer reviewedOxford University PressEuropean CommissionUniversity of HawaiiMinistero dell'Istruzione, dell'Università e della RicercaComisión Nacional de Investigación Científica y Tecnológica (Chile)Fondo Nacional de Desarrollo Científico y Tecnológico (Chile)European Research CouncilAgencia Nacional de Investigación y Desarrollo (Chile)National Science Foundation (US)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/296536reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/101004719info:eu-repo/grantAgreement/EC/H2020/842471info:eu-repo/grantAgreement/EC/H2020/758638Monthly Notices of the Royal Astronomical SocietyThe underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stac744https://doi.org/10.1093/mnras/stac744Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2965362026-05-22T06:33:51Z
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