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dc.contributor.authorGutiérrez, Claudia P.-
dc.contributor.authorPastorello, Andrea-
dc.contributor.authorBersten, Melina C.-
dc.contributor.authorBenetti, Stefano-
dc.contributor.authorOrellana, Mariana Dominga-
dc.contributor.authorFiore, A.-
dc.contributor.authorKaramehmetoglu, Emir-
dc.contributor.authorKravtsov, T.-
dc.contributor.authorReguitti, Andrea-
dc.contributor.authorReynolds, Thomas-
dc.contributor.authorValerin, G.-
dc.contributor.authorMazzali, Paolo-
dc.contributor.authorSullivan, Mark-
dc.contributor.authorCai, Yomgzhi-
dc.contributor.authorElias-Rosa, Nancy-
dc.contributor.authorFraser, Morgan-
dc.contributor.authorHsiao, Eric Y.-
dc.contributor.authorKankare, Erkki-
dc.contributor.authorKotak, R.-
dc.contributor.authorKuncarayakti, H.-
dc.contributor.authorLi, Z.-
dc.contributor.authorMattila, S.-
dc.contributor.authorMo, J.-
dc.contributor.authorMoran, S.-
dc.contributor.authorOchner, P.-
dc.contributor.authorShahbandeh, Melissa-
dc.contributor.authorTomasella, Lina-
dc.contributor.authorWang, X.-
dc.contributor.authorYan, S.-
dc.contributor.authorZhang, J.-
dc.contributor.authorZhang, T.-
dc.contributor.authorStritzinger, Maximilian-
dc.date.accessioned2023-01-30T14:42:59Z-
dc.date.available2023-01-30T14:42:59Z-
dc.date.issued2022-12-
dc.identifier.citationC P Gutiérrez, A Pastorello, M Bersten, S Benetti, M Orellana, A Fiore, E Karamehmetoglu, T Kravtsov, A Reguitti, T M Reynolds, G Valerin, P Mazzali, M Sullivan, Y-Z Cai, N Elias-Rosa, M Fraser, E Y Hsiao, E Kankare, R Kotak, H Kuncarayakti, Z Li, S Mattila, J Mo, S Moran, P Ochner, M Shahbandeh, L Tomasella, X Wang, S Yan, J Zhang, T Zhang, M D Stritzinger, SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O ii lines and a bumpy light curve, Monthly Notices of the Royal Astronomical Society, Volume 517, Issue 2, December 2022, Pages 2056–2075, https://doi.org/10.1093/mnras/stac2747es_ES
dc.identifier.issn0035-8711es_ES
dc.identifier.otherhttps://arxiv.org/abs/2206.01662es_ES
dc.identifier.otherhttps://ui.adsabs.harvard.edu/abs/2022MNRAS.517.2056G/abstract-
dc.identifier.urihttp://rid.unrn.edu.ar/handle/20.500.12049/9575-
dc.description.abstractWe present the analysis of SN 2020wnt, an unusual hydrogen-poor super-luminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterised by an early bump lasting ~5 days, followed by a bright main peak. The SN reaches a peak absolute magnitude of Mr (at max)=-20.52 +/-0.03 mag at ~77.5 days from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O II, but strong lines of C II and Si II are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 Msun and a pre-SN radius of 15 Rsun that experiences a very energetic explosion of 45e51 erg, producing 4 Msun of 56Ni. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out.es_ES
dc.format.extentp. 2056–2075es_ES
dc.language.isoenes_ES
dc.publisherWILEY-BLACKWELL PUBLISHING, INCes_ES
dc.relation.urihttps://academic.oup.com/mnras/article-abstract/517/2/2056/6717660?redirectedFrom=fulltextes_ES
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.titleSN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curvees_ES
dc.typeArticuloes_ES
dc.rights.licenseCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-ND 4.0)-
dc.description.filiationGutiérrez, C. Finnish Centre for Astronomy with ESO (FINCA), FI-20014 University of Turku, Finland.es_ES
dc.description.filiationGutiérrez, C. Tuorla Observatory, Department of Physics and Astronomy, FI-20014 University of Turku, Finland.es_ES
dc.description.filiationPastorello, A. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationBersten, Melina. Instituto de Astrofísica de La Plata, CONICET-UNLP; Argentina.es_ES
dc.description.filiationBenetti, S. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationOrellana, Mariana. Universidad Nacional de Río Negro. Río Negro, Argentina.es_ES
dc.description.filiationOrellana, Mariana. CONICET; Argentina.es_ES
dc.description.filiationFiore, A. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationKaramehmetoglu, E. Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmarkes_ES
dc.description.filiationKravtsov, T. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finlandes_ES
dc.description.filiationReguitti, A. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationReynolds, T. M. Cosmic Dawn Center (DAWN), Denmark; Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmarkes_ES
dc.description.filiationValerin, G. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationMazzali, P. Astrophysics Research Institute, Liverpool John Moores University, UKes_ES
dc.description.filiationSullivan, M. School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UKes_ES
dc.description.filiationCai, Y. Z. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, Chinaes_ES
dc.description.filiationElias-Rosa, N. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationFraser, M. School of Physics, O'Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, Dublin, Irelandes_ES
dc.description.filiationHsiao, E. Y. Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USAes_ES
dc.description.filiationKankare, E. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finlandes_ES
dc.description.filiationKotak, R. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finlandes_ES
dc.description.filiationKuncarayakti, H. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finlandes_ES
dc.description.filiationLi, Z. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, Chinaes_ES
dc.description.filiationLi, Z. School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, Chinaes_ES
dc.description.filiationMattila, S. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finlandes_ES
dc.description.filiationMo, J. Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, Chinaes_ES
dc.description.filiationMoran, S. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finlandes_ES
dc.description.filiationOchner, P. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationShahbandeh, M. Department of Physics, Florida State University, USAes_ES
dc.description.filiationTomasella, L. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italyes_ES
dc.description.filiationWang, X. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, Chinaes_ES
dc.description.filiationYan, S. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, Chinaes_ES
dc.description.filiationZhang, J. Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, Chinaes_ES
dc.description.filiationZhang, T. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, Chinaes_ES
dc.description.filiationStritzinger, M.D. Department of Physics and Astronomy, Aarhus University, Denmarkes_ES
dc.subject.keywordsupernovae: generales_ES
dc.subject.keywordsupernovae: individual: SN 2020wntes_ES
dc.subject.keywordAstrophysics - High Energy Astrophysical Phenomenaes_ES
dc.type.versioninfo:eu-repo/semantics/publishedVersiones_ES
dc.subject.materiaAstronomíaes_ES
dc.origin.lugarDesarrolloUniversidad Nacional de Río Negroes_ES
dc.relation.journalissue517es_ES
dc.description.reviewtruees_ES
dc.description.resumenPresentamos el análisis de SN 2020wnt, una inusual supernova superluminosa pobre en hidrógeno (SLSN-I), con un corrimiento al rojo de 0,032. Las curvas de luz de SN 2020wnt se caracterizan por un aumento temprano que dura ~5 días, seguido de un pico principal brillante. El SN alcanza una magnitud absoluta máxima de Mr (a máx.) = -20,52 +/-0,03 mag a ~77,5 días desde la explosión. Esta magnitud se encuentra en el extremo inferior de la distribución de luminosidad de SLSNe-I, pero el tiempo de subida es uno de los más largos registrados hasta la fecha. A diferencia de otros SLSNe-I, los espectros de SN 2020wnt no muestran OII, pero se detectan fuertes líneas de CII y SiII. Espectroscópicamente, SN 2020wnt se parece al Type Ic SN 2007gr, pero su evolución es significativamente más lenta. Al comparar la curva de luz bolométrica con los modelos hidrodinámicos, encontramos que la luminosidad de SN 2020wnt puede explicarse mediante energía radiactiva. El progenitor de SN 2020wnt es probablemente una estrella masiva y extendida con una masa pre-SN de 80 Msun y un radio pre-SN de 15 Rsun que experimenta una explosión muy enérgica de 45.e51 erg, produciendo 4 Msun de 56Ni. En este marco, el primer pico resulta de una fase de enfriamiento posterior al choque para un progenitor extendido, y el pico principal luminoso se debe a una gran producción de níquel. Estas características son compatibles con el escenario SN de inestabilidad de pares. Sin embargo, notamos que no se puede descartar una contribución significativa de interacción con material circunestelar.es_ES
dc.identifier.doihttps://doi.org/10.1093/mnras/stac2747-
dc.relation.journalTitleMonthly Notices of the Royal Astronomical Societyes_ES
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