The enigmatic double-peaked stripped-envelope SN 2023aew
Kangas, T., et al.
| Autores: | , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/372024 |
| Acceso en línea: | http://hdl.handle.net/10261/372024 |
| Access Level: | acceso abierto |
| Palabra clave: | Accretion Accretion disks Stars: magnetars Stars: mass-loss Supernovae: individual: SN 2023aew |
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The enigmatic double-peaked stripped-envelope SN 2023aew |
| title |
The enigmatic double-peaked stripped-envelope SN 2023aew |
| spellingShingle |
The enigmatic double-peaked stripped-envelope SN 2023aew Kangas, Tuomas Accretion Accretion disks Stars: magnetars Stars: mass-loss Supernovae: individual: SN 2023aew |
| title_short |
The enigmatic double-peaked stripped-envelope SN 2023aew |
| title_full |
The enigmatic double-peaked stripped-envelope SN 2023aew |
| title_fullStr |
The enigmatic double-peaked stripped-envelope SN 2023aew |
| title_full_unstemmed |
The enigmatic double-peaked stripped-envelope SN 2023aew |
| title_sort |
The enigmatic double-peaked stripped-envelope SN 2023aew |
| dc.creator.none.fl_str_mv |
Kangas, Tuomas Elias-Rosa, Nancy Galbany, Lluís Müller-Bravo, Tomás E. Piscarreta, Lara Gutiérrez, Claudia P. |
| author |
Kangas, Tuomas |
| author_facet |
Kangas, Tuomas Elias-Rosa, Nancy Galbany, Lluís Müller-Bravo, Tomás E. Piscarreta, Lara Gutiérrez, Claudia P. |
| author_role |
author |
| author2 |
Elias-Rosa, Nancy Galbany, Lluís Müller-Bravo, Tomás E. Piscarreta, Lara Gutiérrez, Claudia P. |
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author author author author author |
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Royal Society (UK) Science Foundation Ireland Japan Society for the Promotion of Science European Commission Generalitat de Catalunya European Space Agency European Research Council Agencia Estatal de Investigación (España) Ministerio de Ciencia, Innovación y Universidades (España) Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Accretion Accretion disks Stars: magnetars Stars: mass-loss Supernovae: individual: SN 2023aew |
| topic |
Accretion Accretion disks Stars: magnetars Stars: mass-loss Supernovae: individual: SN 2023aew |
| description |
Kangas, T., et al. |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024 2024 2024 |
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info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
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http://hdl.handle.net/10261/372024 |
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http://hdl.handle.net/10261/372024 |
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Inglés |
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Inglés |
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EDP Sciences |
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The enigmatic double-peaked stripped-envelope SN 2023aewKangas, TuomasElias-Rosa, NancyGalbany, LluísMüller-Bravo, Tomás E.Piscarreta, LaraGutiérrez, Claudia P.AccretionAccretion disksStars: magnetarsStars: mass-lossSupernovae: individual: SN 2023aewKangas, T., et al.We present optical and near-infrared photometry and spectroscopy of SN 2023aew and our findings on its remarkable properties. This event, initially resembling a Type IIb supernova (SN), rebrightens dramatically ∼90 d after the first peak, at which time its spectrum transforms into that of a SN Ic. The slowly evolving spectrum specifically resembles a post-peak SN Ic with relatively low line velocities even during the second rise. The second peak, reached 119 d after the first peak, is both more luminous (Mr = −18.75 ± 0.04 mag) and much broader than those of typical SNe Ic. Blackbody fits to SN 2023aew indicate that the photosphere shrinks almost throughout its observed evolution, and the second peak is caused by an increasing temperature. Bumps in the light curve after the second peak suggest interaction with circumstellar matter (CSM) or possibly accretion. We consider several scenarios for producing the unprecedented behavior of SN 2023aew. Two separate SNe, either unrelated or from the same binary system, require either an incredible coincidence or extreme fine-tuning. A pre-SN eruption followed by a SN requires an extremely powerful, SN-like eruption (consistent with ∼1051 erg) and is also disfavored. We therefore consider only the first peak a true stellar explosion. The observed evolution is difficult to reproduce if the second peak is dominated by interaction with a distant CSM shell. A delayed internal heating mechanism is more likely, but emerging embedded interaction with a CSM disk should be accompanied by CSM lines in the spectrum, which are not observed, and is difficult to hide long enough. A magnetar central engine requires a delayed onset to explain the long time between the peaks. Delayed fallback accretion onto a black hole may present the most promising scenario, but we cannot definitively establish the power source.HK was funded by the Research Council of Finland projects 324504, 328898, and 353019. TN acknowledges support from the Research Council of Finland projects 324504 and 328898. RK acknowledges support via Research Council of Finland (grant 340613). MF is supported by a Royal Society – Science Foundation Ireland University Research Fellowship. HFS is supported by the Eric and Wendy Schmidt A.I. in Science Fellowship. KM acknowledges support from JSPS KAKENHI grant (JP20H04737) and the JSPS Open Partnership Bilateral Joint Research Project between Japan and Finland (JPJSBP120229923). MDS is funded by the Independent Research Fund Denmark (IRFD, grant number 10.46540/2032-00022B. CPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. Y-ZC is supported by the National Natural Science Foundation of China (NSFC, Grant No. 12303054), the Yunnan Fundamental Research Projects (Grant No. 202401AU070063) and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). MP acknowledges support from a UK Research and Innovation Fellowship (MR/T020784/1). PC acknowledges support via Research Council of Finland grant 340613. SM acknowledges support from the Research Council of Finland project 350458. NER, AP, SB, AR and GV acknowledge support from the PRIN-INAF 2022, ‘Shedding light on the nature of gap transients: from the observations to the models’. NER also acknowledges partial support from MIUR, PRIN 2017 (grant 20179ZF5KS). AR also acknowledges financial support from the INAF GRAWITA Large Program Grant. We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (http://gsaweb.ast.cam.ac.uk/alerts). The Starlink software (Currie et al. 2014) is currently supported by the East Asian Observatory. Partially based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT. This study is 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. Access to the Las Cumbres Observatory was made possible via an allocation by OPTICON (program 22A/012, PI Stritzinger). This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 101004719. The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from Indo-US Science and Technology Forum and the Science and Engineering Research Board, Department of Science and Technology, Government of India. It is located at the Indian Astronomical Observatory (IAO, Hanle). We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operation of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/. Operation of Nayuta telescope and NIC is partially supported by the Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) program funded by the MEXT of Japan. The spectra taken by the Seimei telescope are obtained under the KASTOR (Kanata And Seimei Transient Observation Regime) campaign. The Seimei telescope at the Okayama Observatory is jointly operated by Kyoto University and the Astronomical Observatory of Japan (NAOJ), with assistance provided by the OISTER program.With funding from the Spanish government through the "Unit of Excellence Maria de Maeztu" accreditation (CEX2020-001058-M).Peer reviewedEDP SciencesRoyal Society (UK)Science Foundation IrelandJapan Society for the Promotion of ScienceEuropean CommissionGeneralitat de CatalunyaEuropean Space AgencyEuropean Research CouncilAgencia Estatal de Investigación (España)Ministerio de Ciencia, Innovación y Universidades (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202420242024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/372024reponame: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##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/801370info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2020-001058-Minfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-115253GA-I00info:eu-repo/grantAgreement/EC/H2020/101004719https://doi.org/10.1051/0004-6361/202449420Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3720242026-05-22T06:33:51Z |
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