Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst
Long γ-ray bursts are associated with energetic, broad-lined, stripped-envelope supernovae and as such mark the death of massive stars. The scarcity of such events nearby and the brightness of the γ-ray burst afterglow, which dominates the emission in the first few days after the burst, have so far...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2019 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/194415 |
| Acceso en línea: | http://hdl.handle.net/10261/194415 |
| Access Level: | acceso abierto |
| Palabra clave: | High-energy astrophysics Transient astrophysical phenomena |
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Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| title |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| spellingShingle |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst Izzo, L. High-energy astrophysics Transient astrophysical phenomena |
| title_short |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| title_full |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| title_fullStr |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| title_full_unstemmed |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| title_sort |
Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst |
| dc.creator.none.fl_str_mv |
Izzo, L. Ugarte Postigo, Antonio de Maeda, K. Thöne, Cristina Carina Kann, D.A. Della Valle, M. Sagues Carracedo, A. Michałowski, M. J. Schady, P. Schmidl, S. Selsing, J. Starling, R.L.C. Suzuki, A. Bensch, K. Bolmer, J. Campana, S. Cano, Z. Covino, Stefano Fynbo, J. P. U. Hartmann, D.H. Heintz, K.E. Hjorth, Jens Japelj, J. Kaminski, K. Kaper, L. Kouveliotou, C. Kruzynski, M. Kwiatkowski, T. Leloudas, Giorgos Levan, A.J. Malesani, D.B. Michałowski, T. Piranomonte, S. Pugliese, G. Rossi, A. Sánchez Ramírez, Rubén Schulze, S. Steeghs, D. Tanvir, N.R. Ulaczyk, K. Vergani, S.D. Wiersema, K. |
| author |
Izzo, L. |
| author_facet |
Izzo, L. Ugarte Postigo, Antonio de Maeda, K. Thöne, Cristina Carina Kann, D.A. Della Valle, M. Sagues Carracedo, A. Michałowski, M. J. Schady, P. Schmidl, S. Selsing, J. Starling, R.L.C. Suzuki, A. Bensch, K. Bolmer, J. Campana, S. Cano, Z. Covino, Stefano Fynbo, J. P. U. Hartmann, D.H. Heintz, K.E. Hjorth, Jens Japelj, J. Kaminski, K. Kaper, L. Kouveliotou, C. Kruzynski, M. Kwiatkowski, T. Leloudas, Giorgos Levan, A.J. Malesani, D.B. Michałowski, T. Piranomonte, S. Pugliese, G. Rossi, A. Sánchez Ramírez, Rubén Schulze, S. Steeghs, D. Tanvir, N.R. Ulaczyk, K. Vergani, S.D. Wiersema, K. |
| author_role |
author |
| author2 |
Ugarte Postigo, Antonio de Maeda, K. Thöne, Cristina Carina Kann, D.A. Della Valle, M. Sagues Carracedo, A. Michałowski, M. J. Schady, P. Schmidl, S. Selsing, J. Starling, R.L.C. Suzuki, A. Bensch, K. Bolmer, J. Campana, S. Cano, Z. Covino, Stefano Fynbo, J. P. U. Hartmann, D.H. Heintz, K.E. Hjorth, Jens Japelj, J. Kaminski, K. Kaper, L. Kouveliotou, C. Kruzynski, M. Kwiatkowski, T. Leloudas, Giorgos Levan, A.J. Malesani, D.B. Michałowski, T. Piranomonte, S. Pugliese, G. Rossi, A. Sánchez Ramírez, Rubén Schulze, S. Steeghs, D. Tanvir, N.R. Ulaczyk, K. Vergani, S.D. Wiersema, K. |
| 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 author author author |
| dc.contributor.none.fl_str_mv |
Japan Society for the Promotion of Science Science and Technology Facilities Council (UK) Agenzia Spaziale Italiana Villum Fonden Icelandic Research Fund Fundação de Amparo à Pesquisa do Estado de São Paulo National Science Centre (Poland) Ministerio de Economía y Competitividad (España) European Commission Ministry of Education, Culture, Sports, Science and Technology (Japan) Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
High-energy astrophysics Transient astrophysical phenomena |
| topic |
High-energy astrophysics Transient astrophysical phenomena |
| description |
Long γ-ray bursts are associated with energetic, broad-lined, stripped-envelope supernovae and as such mark the death of massive stars. The scarcity of such events nearby and the brightness of the γ-ray burst afterglow, which dominates the emission in the first few days after the burst, have so far prevented the study of the very early evolution of supernovae associated with γ-ray bursts. In hydrogen-stripped supernovae that are not associated with γ-ray bursts, an excess of high-velocity (roughly 30,000 kilometres per second) material has been interpreted as a signature of a choked jet, which did not emerge from the progenitor star and instead deposited all of its energy in a thermal cocoon. Here we report multi-epoch spectroscopic observations of the supernova SN 2017iuk, which is associated with the γ-ray burst GRB 171205A. Our spectra display features at extremely high expansion velocities (around 115,000 kilometres per second) within the first day after the burst. Using spectral synthesis models developed for SN 2017iuk, we show that these features are characterized by chemical abundances that differ from those observed in the ejecta of SN 2017iuk at later times. We further show that the high-velocity features originate from the mildly relativistic hot cocoon that is generated by an ultra-relativistic jet within the γ-ray burst expanding and decelerating into the medium that surrounds the progenitor star. This cocoon rapidly becomes transparent and is outshone by the supernova emission, which starts to dominate the emission three days after the burst. © 2019, Springer Nature Limited. |
| publishDate |
2019 |
| dc.date.none.fl_str_mv |
2019 2019 2019 2019 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Postprint info:eu-repo/semantics/acceptedVersion |
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article |
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acceptedVersion |
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http://hdl.handle.net/10261/194415 |
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http://hdl.handle.net/10261/194415 |
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Inglés |
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info:eu-repo/semantics/openAccess |
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openAccess |
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Nature Publishing Group |
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Nature Publishing Group |
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reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
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Consejo Superior de Investigaciones Científicas (CSIC) |
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Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burstIzzo, L.Ugarte Postigo, Antonio deMaeda, K.Thöne, Cristina CarinaKann, D.A.Della Valle, M.Sagues Carracedo, A.Michałowski, M. J.Schady, P.Schmidl, S.Selsing, J.Starling, R.L.C.Suzuki, A.Bensch, K.Bolmer, J.Campana, S.Cano, Z.Covino, StefanoFynbo, J. P. U.Hartmann, D.H.Heintz, K.E.Hjorth, JensJapelj, J.Kaminski, K.Kaper, L.Kouveliotou, C.Kruzynski, M.Kwiatkowski, T.Leloudas, GiorgosLevan, A.J.Malesani, D.B.Michałowski, T.Piranomonte, S.Pugliese, G.Rossi, A.Sánchez Ramírez, RubénSchulze, S.Steeghs, D.Tanvir, N.R.Ulaczyk, K.Vergani, S.D.Wiersema, K.High-energy astrophysicsTransient astrophysical phenomenaLong γ-ray bursts are associated with energetic, broad-lined, stripped-envelope supernovae and as such mark the death of massive stars. The scarcity of such events nearby and the brightness of the γ-ray burst afterglow, which dominates the emission in the first few days after the burst, have so far prevented the study of the very early evolution of supernovae associated with γ-ray bursts. In hydrogen-stripped supernovae that are not associated with γ-ray bursts, an excess of high-velocity (roughly 30,000 kilometres per second) material has been interpreted as a signature of a choked jet, which did not emerge from the progenitor star and instead deposited all of its energy in a thermal cocoon. Here we report multi-epoch spectroscopic observations of the supernova SN 2017iuk, which is associated with the γ-ray burst GRB 171205A. Our spectra display features at extremely high expansion velocities (around 115,000 kilometres per second) within the first day after the burst. Using spectral synthesis models developed for SN 2017iuk, we show that these features are characterized by chemical abundances that differ from those observed in the ejecta of SN 2017iuk at later times. We further show that the high-velocity features originate from the mildly relativistic hot cocoon that is generated by an ultra-relativistic jet within the γ-ray burst expanding and decelerating into the medium that surrounds the progenitor star. This cocoon rapidly becomes transparent and is outshone by the supernova emission, which starts to dominate the emission three days after the burst. © 2019, Springer Nature Limited.L.I. acknowledges support from funding associated with Juan de la Cierva Incorporacion fellowship IJCI-2016-30940. L.I., A.d.U.P., C.C.T. and D.A.K. acknowledge support from the Spanish research project AYA2017-89384-P. A.d.U.P. acknowledges support from funding associated with Ramon y Cajal fellowship RyC-2012-09975. C.C.T. acknowledges support from funding associated with Ramon y Cajal fellowship RyC-2012-09984. D.A.K. acknowledges support from funding associated with Juan de la Cierva Incorporacion fellowship IJCI-2015-26153. K.M. acknowledges support from JSPS Kakenhi grants (18H05223, 18H04585 and 17H02864). S. Schmidl acknowledges support from grant DFG Klose 766/16-3 and discussions with S. Klose. R.L.C.S. acknowledges funding from STFC. M.J.M. acknowledges the support of the National Science Centre, Poland, through POLONEZ grant 2015/19/P/ST9/04010; this project has received funding from the European Union's Horizon 2020 research and innovation programme under Marie Sklodowska-Curie grant agreement number 665778. R.S.-R. acknowledges support from ASI (Italian Space Agency) through contract number 2015-046-R.0 and from the European Union's Horizon 2020 programme under the AHEAD project (grant agreement number 654215). The Cosmic Dawn Center is funded by the DNRF. J.H. was supported by a VILLUM FONDEN Investigator grant (project number 16599). G.L. was supported by a research grant from VILLUM FONDEN (project number 19054). K.E.H. acknowledges support by a Project Grant (162948-051) from The Icelandic Research fund. J.J. and L.K. acknowledge support from NOVA and NWO-FAPESP grant for advanced instrumentation in astronomy.Peer ReviewedNature Publishing GroupJapan Society for the Promotion of ScienceScience and Technology Facilities Council (UK)Agenzia Spaziale ItalianaVillum FondenIcelandic Research FundFundação de Amparo à Pesquisa do Estado de São PauloNational Science Centre (Poland)Ministerio de Economía y Competitividad (España)European CommissionMinistry of Education, Culture, Sports, Science and Technology (Japan)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2019201920192019info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/194415reponame: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##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/IJCI-2016-30940info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/IJCI-2015-26153info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-89384-Pinfo:eu-repo/grantAgreement/EC/H2020/654215info:eu-repo/grantAgreement/EC/H2020/665778http:dx.doi.org/10.1038/s41586-018-0826-3Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/1944152026-05-22T06:33:51Z |
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