The metamorphosis of the Type Ib SN 2019yvr: late-time interaction

L. Ferrari et al.

Detalles Bibliográficos
Autores: Ferrari, Lucía, Galbany, Lluís, Gutiérrez, Claudia P., Müller-Bravo, Tomás E.
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:10261/357896
Acceso en línea:http://hdl.handle.net/10261/357896
Access Level:acceso abierto
Palabra clave:Supernovae: general
Supernovae: individual: SN 2019yvr
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dc.title.none.fl_str_mv The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
title The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
spellingShingle The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
Ferrari, Lucía
Supernovae: general
Supernovae: individual: SN 2019yvr
title_short The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
title_full The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
title_fullStr The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
title_full_unstemmed The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
title_sort The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
dc.creator.none.fl_str_mv Ferrari, Lucía
Galbany, Lluís
Gutiérrez, Claudia P.
Müller-Bravo, Tomás E.
author Ferrari, Lucía
author_facet Ferrari, Lucía
Galbany, Lluís
Gutiérrez, Claudia P.
Müller-Bravo, Tomás E.
author_role author
author2 Galbany, Lluís
Gutiérrez, Claudia P.
Müller-Bravo, Tomás E.
author2_role author
author
author
dc.contributor.none.fl_str_mv Japan Society for the Promotion of Science
National Natural Science Foundation of China
Istituto Nazionale di Astrofisica
Agencia Estatal de Investigación (España)
Ministerio de Ciencia e Innovación (España)
European Commission
Ministerio de Ciencia, Innovación y Universidades (España)
European Research Council
Consejo Superior de Investigaciones Científicas (España)
Generalitat de Catalunya
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Supernovae: general
Supernovae: individual: SN 2019yvr
topic Supernovae: general
Supernovae: individual: SN 2019yvr
description L. Ferrari et al.
publishDate 2024
dc.date.none.fl_str_mv 2024
2024
2024
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/357896
url http://hdl.handle.net/10261/357896
dc.language.none.fl_str_mv Inglés
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The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnrasl/slad195
https://doi.org/10.1093/mnrasl/slad195
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dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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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)
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spelling The metamorphosis of the Type Ib SN 2019yvr: late-time interactionFerrari, LucíaGalbany, LluísGutiérrez, Claudia P.Müller-Bravo, Tomás E.Supernovae: generalSupernovae: individual: SN 2019yvrL. Ferrari et al.We present observational evidence of late-time interaction between the ejecta of the hydrogen-poor Type Ib supernova (SN) 2019yvr and hydrogen-rich circumstellar material (CSM), similar to the Type Ib SN 2014C. A narrow H α emission line appears simultaneously with a break in the light-curve decline rate at around 80–100 d after explosion. From the interaction delay and the ejecta velocity, under the assumption that the CSM is detached from the progenitor, we estimate the CSM inner radius to be located at ∼6.5–9.1 × 1015 cm. The H α emission line persists throughout the nebular phase at least up to +420 d post-explosion, with a full width at half maximum of ∼2000 km s−1. Assuming a steady mass-loss, the estimated mass-loss rate from the luminosity of the H α line is ∼3–7 × 10−5 M⊙ yr−1. From hydrodynamical modelling and analysis of the nebular spectra, we find a progenitor He-core mass of 3–4 M⊙, which would imply an initial mass of 13–15 M⊙. Our result supports the case of a relatively low-mass progenitor possibly in a binary system as opposed to a higher mass single star undergoing a luminous blue variable phase.The Finnish National Agency for Education (EDUFI) supported this research project through an EDUFI Fellowship. HK was funded by the Research Council of Finland projects 324504, 328898, and 353019. MDS is funded by the Independent Research Fund Denmark (IRFD) via Project 2 grant 10.46540/2032-00022B. KM acknowledges support from the Japan Society for the Promotion of Science (JSPS) KAKENHI grant (JP20H00174) and by the JSPS Open Partnership Bilateral Joint Research Project between Japan and Finland (JPJSBP120229923). NUTS is funded in part by the Instrument center for Danish Astrophysics (IDA). LCOGT network data were obtained through OPTICON (PI Stritzinger, programme ID 2020A/031) and NOAO (PI Bose, programme ID NOAO2020A-017) time allocations. 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. Data were also obtained 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 work includes data collected at ESO via programme IDs 1103.D-0328, 0105.D-0511, and 1106.D-0811. We thank the Subaru staff for the data taken by the Subaru Telescope (S19B-054); the authors acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. YZC is supported by the National Natural Science Foundation of China (NSFC,; grant no. 12303054) and the International Centre of Supernovae, Yunnan Key Laboratory (no. 202302AN360001). AP is supported by the PRIN-INAF 2022 project ‘Shedding light on the nature of gap transients: from the observations to the models’. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Social Fund (ESF) ‘Investing in your future’ under the 2019 Ramón y Cajal programme RYC2019-027683-Iand the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the programme Unidad de Excelencia María de Maeztu CEX2020-001058-M. 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 programme Unidad de Excelencia María de Maeztu CEX2020-001058-M. TEMB acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Union Next Generation EU/PRTR funds under the 2021 Juan de la Cierva programme FJC2021-047124-Iand the PID2020-115253GA-I00HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the programme Unidad de Excelencia María de Maeztu CEX2020-001058-M. SM acknowledges support from the Research Council of Finland project 350458. MN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 948381) and by UK Space Agency grant no. ST/Y000692/1. GP acknowledges support from ANID through Millennium Science Initiative Programs ICN12_009.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2020-001058-M).Peer reviewedOxford University PressJapan Society for the Promotion of ScienceNational Natural Science Foundation of ChinaIstituto Nazionale di AstrofisicaAgencia Estatal de Investigación (España)Ministerio de Ciencia e Innovación (España)European CommissionMinisterio de Ciencia, Innovación y Universidades (España)European Research CouncilConsejo Superior de Investigaciones Científicas (España)Generalitat de CatalunyaConsejo 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/10261/357896reponame: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/AEI//RYC2019-027683-Iinfo: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/H2020/948381The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnrasl/slad195https://doi.org/10.1093/mnrasl/slad195Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3578962026-05-22T06:33:51Z
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