SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve

• Autores: Gutiérrez, Claudia P.; Pastorello, Andrea; Bersten, Melina C.; Benetti, Stefano; Orellana, Mariana Dominga; Fiore, A.; Karamehmetoglu, Emir; Kravtsov, T.; Reguitti, Andrea; Reynolds, Thomas; Valerin, G.; Mazzali, Paolo; Sullivan, Mark; Cai, Yomgzhi; Elias-Rosa, Nancy; Fraser, Morgan; Hsiao, Eric Y.; Kankare, Erkki; Kotak, R.; Kuncarayakti, H.; Li, Z.; Mattila, S.; Mo, J.; Moran, S.; Ochner, P.; Shahbandeh, Melissa; Tomasella, Lina; Wang, X.; Yan, S.; Zhang, J.; Zhang, T.; Stritzinger, Maximilian
• Año de publicación: 2022
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: Astronomía; supernovae: general; supernovae: individual: SN 2020wnt; Astrophysics - High Energy Astrophysical Phenomena; Astronomía
• Institución: Universidad Nacional de Río Negro

Fil: Gutiérrez, C. Finnish Centre for Astronomy with ESO (FINCA), FI-20014 University of Turku, Finland.
Fil: Gutiérrez, C. Tuorla Observatory, Department of Physics and Astronomy, FI-20014 University of Turku, Finland.
Fil: Pastorello, A. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Bersten, Melina. Instituto de Astrofísica de La Plata, CONICET-UNLP; Argentina.
Fil: Benetti, S. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Orellana, Mariana. Universidad Nacional de Río Negro. Río Negro, Argentina.
Fil: Orellana, Mariana. CONICET; Argentina.
Fil: Fiore, A. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Karamehmetoglu, E. Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
Fil: Kravtsov, T. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
Fil: Reguitti, A. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Reynolds, T. M. Cosmic Dawn Center (DAWN), Denmark; Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmark
Fil: Valerin, G. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Mazzali, P. Astrophysics Research Institute, Liverpool John Moores University, UK
Fil: Sullivan, M. School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK
Fil: Cai, Y. Z. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
Fil: Elias-Rosa, N. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Fraser, M. School of Physics, O'Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, Dublin, Ireland
Fil: Hsiao, E. Y. Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA
Fil: Kankare, E. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finland
Fil: Kotak, R. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finland
Fil: Kuncarayakti, H. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finland
Fil: Li, Z. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
Fil: Li, Z. School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, China
Fil: Mattila, S. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finland
Fil: Mo, J. Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, China
Fil: Moran, S. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Finland
Fil: Ochner, P. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Shahbandeh, M. Department of Physics, Florida State University, USA
Fil: Tomasella, L. INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
Fil: Wang, X. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
Fil: Yan, S. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
Fil: Zhang, J. Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China
Fil: Zhang, T. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
Fil: Stritzinger, M.D. Department of Physics and Astronomy, Aarhus University, Denmark
We 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.
Presentamos 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.