SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn
We present observations of supernova (SN) 2017ens, discovered by the ATLAS survey and identified as a hot blue object through the GREAT program. The redshift z = 0.1086 implies a peak brightness of M = -21.1 mag, placing the object within the regime of superluminous supernovae. We observe a dramatic...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Tipo de documento: | artigo |
| Estado: | Versión aceptada para publicación |
| Data de publicação: | 2018 |
| País: | España |
| Recursos: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositório: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/216265 |
| Acesso em linha: | http://hdl.handle.net/10261/216265 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Supernovae: general Supernovae: individual (SN 2017ens) |
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SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| title |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| spellingShingle |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn Chen, T. W. Supernovae: general Supernovae: individual (SN 2017ens) |
| title_short |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| title_full |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| title_fullStr |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| title_full_unstemmed |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| title_sort |
SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn |
| dc.creator.none.fl_str_mv |
Chen, T. W. Inserra, Cosimo Fraser, Morgan Moriya, T. J. Schady, P. Schweyer, T. Filippenko, Alexei V. Perley, D.A. Ruiter, A. J. Seitenzahl, I. Sollerman, J. Taddia, Francesco Anderson, Joseph P. Foley, R. J. Jerkstrand, A. Ngeow, C. -C. Pan, Y. -C. Pastorello, Andrea Points, S. Smartt, S. J. Smith, Ken W. Taubenberger, S. Wiseman, Philip Young, D. R. Benetti, S. Berton, M. Bufano, F. Clark, P. Della Valle, M. Galbany, Lluís Gal-Yam, Avishay Gromadzki, M. Gutiérrez, Claudia P. Heinze, A. Kankare, E. Kilpatrick, C. D. Kuncarayakti, Hanindyo Leloudas, Giorgos Lin, Zhong-Yi Maguire, Kate Mazzali, Paolo A. McBrien, O. Prentice, S.J. Rau, A. Rest, Armin Siebert, M. R. Stalder, B. Tonry, J. L. Yu, P. -C. |
| author |
Chen, T. W. |
| author_facet |
Chen, T. W. Inserra, Cosimo Fraser, Morgan Moriya, T. J. Schady, P. Schweyer, T. Filippenko, Alexei V. Perley, D.A. Ruiter, A. J. Seitenzahl, I. Sollerman, J. Taddia, Francesco Anderson, Joseph P. Foley, R. J. Jerkstrand, A. Ngeow, C. -C. Pan, Y. -C. Pastorello, Andrea Points, S. Smartt, S. J. Smith, Ken W. Taubenberger, S. Wiseman, Philip Young, D. R. Benetti, S. Berton, M. Bufano, F. Clark, P. Della Valle, M. Galbany, Lluís Gal-Yam, Avishay Gromadzki, M. Gutiérrez, Claudia P. Heinze, A. Kankare, E. Kilpatrick, C. D. Kuncarayakti, Hanindyo Leloudas, Giorgos Lin, Zhong-Yi Maguire, Kate Mazzali, Paolo A. McBrien, O. Prentice, S.J. Rau, A. Rest, Armin Siebert, M. R. Stalder, B. Tonry, J. L. Yu, P. -C. |
| author_role |
author |
| author2 |
Inserra, Cosimo Fraser, Morgan Moriya, T. J. Schady, P. Schweyer, T. Filippenko, Alexei V. Perley, D.A. Ruiter, A. J. Seitenzahl, I. Sollerman, J. Taddia, Francesco Anderson, Joseph P. Foley, R. J. Jerkstrand, A. Ngeow, C. -C. Pan, Y. -C. Pastorello, Andrea Points, S. Smartt, S. J. Smith, Ken W. Taubenberger, S. Wiseman, Philip Young, D. R. Benetti, S. Berton, M. Bufano, F. Clark, P. Della Valle, M. Galbany, Lluís Gal-Yam, Avishay Gromadzki, M. Gutiérrez, Claudia P. Heinze, A. Kankare, E. Kilpatrick, C. D. Kuncarayakti, Hanindyo Leloudas, Giorgos Lin, Zhong-Yi Maguire, Kate Mazzali, Paolo A. McBrien, O. Prentice, S.J. Rau, A. Rest, Armin Siebert, M. R. Stalder, B. Tonry, J. L. Yu, P. -C. |
| 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 author author author author author author author |
| dc.contributor.none.fl_str_mv |
Alexander von Humboldt Foundation Science Foundation Ireland Tabasgo Foundation Miller Institute for Basic Research in Science Australian Research Council European Research Council Science and Technology Facilities Council (UK) National Science Centre (Poland) National Science Foundation (US) Ministry of Science and Technology (Taiwan) Istituto Nazionale di Astrofisica Israel Science Foundation W. M. Keck Foundation German Research Foundation Christopher R. Redlich Fund Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Supernovae: general Supernovae: individual (SN 2017ens) |
| topic |
Supernovae: general Supernovae: individual (SN 2017ens) |
| description |
We present observations of supernova (SN) 2017ens, discovered by the ATLAS survey and identified as a hot blue object through the GREAT program. The redshift z = 0.1086 implies a peak brightness of M = -21.1 mag, placing the object within the regime of superluminous supernovae. We observe a dramatic spectral evolution, from initially being blue and featureless, to later developing features similar to those of the broadlined Type Ic SN 1998bw, and finally showing ∼2000 km s wide Hα and Hβ emission. Relatively narrow Balmer emission (reminiscent of a SN IIn) is present at all times. We also detect coronal lines, indicative of a dense circumstellar medium. We constrain the progenitor wind velocity to ∼50-60 km s based on P-Cygni profiles, which is far slower than those present in Wolf-Rayet stars. This may suggest that the progenitor passed through a luminous blue variable phase, or that the wind is instead from a binary companion red supergiant star. At late times we see the ∼2000 km s wide Hα emission persisting at high luminosity (∼3 × 10 erg s) for at least 100 day, perhaps indicative of additional mass loss at high velocities that could have been ejected by a pulsational pair instability. © 2018. The American Astronomical Society. All rights reserved. |
| publishDate |
2018 |
| dc.date.none.fl_str_mv |
2018 2020 2020 2020 |
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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/10261/216265 |
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http://hdl.handle.net/10261/216265 |
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Inglés |
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Inglés |
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info:eu-repo/semantics/openAccess |
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openAccess |
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IOP Publishing |
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IOP Publishing |
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reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
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SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IInChen, T. W.Inserra, CosimoFraser, MorganMoriya, T. J.Schady, P.Schweyer, T.Filippenko, Alexei V.Perley, D.A.Ruiter, A. J.Seitenzahl, I.Sollerman, J.Taddia, FrancescoAnderson, Joseph P.Foley, R. J.Jerkstrand, A.Ngeow, C. -C.Pan, Y. -C.Pastorello, AndreaPoints, S.Smartt, S. J.Smith, Ken W.Taubenberger, S.Wiseman, PhilipYoung, D. R.Benetti, S.Berton, M.Bufano, F.Clark, P.Della Valle, M.Galbany, LluísGal-Yam, AvishayGromadzki, M.Gutiérrez, Claudia P.Heinze, A.Kankare, E.Kilpatrick, C. D.Kuncarayakti, HanindyoLeloudas, GiorgosLin, Zhong-YiMaguire, KateMazzali, Paolo A.McBrien, O.Prentice, S.J.Rau, A.Rest, ArminSiebert, M. R.Stalder, B.Tonry, J. L.Yu, P. -C.Supernovae: generalSupernovae: individual (SN 2017ens)We present observations of supernova (SN) 2017ens, discovered by the ATLAS survey and identified as a hot blue object through the GREAT program. The redshift z = 0.1086 implies a peak brightness of M = -21.1 mag, placing the object within the regime of superluminous supernovae. We observe a dramatic spectral evolution, from initially being blue and featureless, to later developing features similar to those of the broadlined Type Ic SN 1998bw, and finally showing ∼2000 km s wide Hα and Hβ emission. Relatively narrow Balmer emission (reminiscent of a SN IIn) is present at all times. We also detect coronal lines, indicative of a dense circumstellar medium. We constrain the progenitor wind velocity to ∼50-60 km s based on P-Cygni profiles, which is far slower than those present in Wolf-Rayet stars. This may suggest that the progenitor passed through a luminous blue variable phase, or that the wind is instead from a binary companion red supergiant star. At late times we see the ∼2000 km s wide Hα emission persisting at high luminosity (∼3 × 10 erg s) for at least 100 day, perhaps indicative of additional mass loss at high velocities that could have been ejected by a pulsational pair instability. © 2018. The American Astronomical Society. All rights reserved.T.W.C. acknowledges Thomas. Kruhler for the X-Shooter data reduction, Lin Yan and Claes Fransson for providing comparison spectra, Jason Spyromilio for useful discussions, Chien-Hsiu. Lee and You-Hua. Chu for coordinating observational resources, and funding from the Alexander von Humboldt Foundation. M.F. acknowledges the support of a Royal Society-Science Foundation Ireland University Research Fellowship. P.S. acknowledges support through the Sofia Kovalevskaja Award (Alexander von Humboldt Foundation). A.V.F. is grateful for the support of the TABASGO Foundation, the Christopher R. Redlich fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). A.J.R. and I.R.S. are supported by the Australian Research Council through grants FT170100243 and FT160100028, respectively. F.T. and J.S. acknowledge support from the KAW Foundation. S.J.S. acknowledges funding from the European Research Council Grant agreement #291222 and STFC grant ST/P000312/1. M.G. is supported by Polish National Science Centre grant OPUS 2015/17/B/ST9/03167. K.M. acknowledges support from the UK STFC through an Ernest Rutherford Fellowship and from a Horizon 2020 ERC Starting Grant (#758638). L.G. was supported in part by US NSF grant AST-1311862. C.P.G. acknowledges support from EU/FP7-ERC grant #615929. Z.Y.L., C.C.N., and P.C.Y. are grateful for funding from MoST (Taiwan) under grants 105-2112-M-008-002-MY3, 104-2923-M-008-004-MY5, and 106-2112-M-008-007. A.P. and S.B. are partially supported by PRIN-INAF 2017 "Toward the SKA and CTA era: discovery, localization, and physics of transient sources" (P.I.: Giroletti). A.G.-Y. is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program, and a Kimmel award. Part of the funding for GROND was generously granted from the Leibniz Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). Some observations were made with the Nordic Optical Telescope using ALFOSC. This publication has made use of data collected at Lulin Observatory, partly supported by MoST grant 105-2112-M-008-024-MY3. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation.IOP PublishingAlexander von Humboldt FoundationScience Foundation IrelandTabasgo FoundationMiller Institute for Basic Research in ScienceAustralian Research CouncilEuropean Research CouncilScience and Technology Facilities Council (UK)National Science Centre (Poland)National Science Foundation (US)Ministry of Science and Technology (Taiwan)Istituto Nazionale di AstrofisicaIsrael Science FoundationW. M. Keck FoundationGerman Research FoundationChristopher R. Redlich FundConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2020202020182020info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/216265reponame: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/H2020/291222info:eu-repo/grantAgreement/EC/H2020/758638info:eu-repo/grantAgreement/EC/FP7/615929info:eu-repo/grantAgreement/EC/H2020/725161http://dx.doi.org/10.3847/2041-8213/aaeb2eSíinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2162652026-05-22T06:33:51Z |
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