SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O <scp>ii</scp> lines and a bumpy light curve-Reference-Cited by-同舟云学术

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

Published:2022-09-26 Issue:2 Volume:517 Page:2056-2075
ISSN:0035-8711
Container-title:Monthly Notices of the Royal Astronomical Society
language:en
Short-container-title:

Author:

Gutiérrez C P¹²^ORCID,Pastorello A³^ORCID,Bersten M⁴⁵⁶,Benetti S³^ORCID,Orellana M⁷⁸,Fiore A³⁹¹⁰,Karamehmetoglu E¹¹^ORCID,Kravtsov T²,Reguitti A³¹²¹³^ORCID,Reynolds T M¹⁴¹⁵^ORCID,Valerin G³¹⁶,Mazzali P¹⁷¹⁸,Sullivan M¹⁹^ORCID,Cai Y-Z²⁰^ORCID,Elias-Rosa N³²¹^ORCID,Fraser M²²^ORCID,Hsiao E Y²³^ORCID,Kankare E²²⁴^ORCID,Kotak R²,Kuncarayakti H¹²,Li Z²⁵²⁶,Mattila S²,Mo J²⁷,Moran S²,Ochner P³¹⁶,Shahbandeh M²³^ORCID,Tomasella L³^ORCID,Wang X²⁰²⁷,Yan S²⁰,Zhang J²⁸²⁹,Zhang T²⁵²⁶,Stritzinger M D¹¹^ORCID

Affiliation:

1. Finnish Centre for Astronomy with ESO (FINCA) , University of Turku, FI-20014 Turku, Finland

2. Tuorla Observatory, Department of Physics and Astronomy , University of Turku, FI-20014 Turku, Finland

3. INAF – Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, Italy

4. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, Argentina

5. Instituto de Astrofísica de La Plata (IALP), CCT-CONICET-UNLP , Paseo del Bosque S/N, B1900FWA La Plata, Argentina

6. Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan

7. Universidad Nacional de Río Negro. Sede Andina , Mitre 630 (8400), Bariloche, Argentina

8. Consejo Nacional de Investigaciones Científicas y Tecnicas (CONICET) , Argentina

9. European Centre for Theoretical Studies in Nuclear Physics and Related Areas (ECT*) , Fondazione Bruno Kessler, I-38123 Trento, Italy

10. INFN – TIFPA, Trento Institute for Fundamental Physics and Applications , Via Sommarive 14, I-38123 Trento, Italy

11. Department of Physics and Astronomy, Aarhus University , Ny Munkegade 120, DK-8000 Aarhus C, Denmark

12. Departamento de Ciencias Físicas – Universidad Andrés Bello , Avda. República 252, Santiago, Chile

13. Millennium Institute of Astrophysics , Nuncio Monsenor Sótero Sanz 100, Providencia, Santiago, Chile

14. Cosmic Dawn Center (DAWN) , Denmark

15. Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark

16. Department of Physics and Astronomy G. Galilei, University of Padova , Vicolo dell’Osservatorio 3, I-35122 Padova, Italy

17. Astrophysics Research Institute, Liverpool John Moores University , IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK

18. Max-Planck-Institut für Astrophysik , Karl-Schwarzschild Str. 1, D-85748 Garching, Germany

19. School of Physics and Astronomy, University of Southampton , Southampton SO17 1BJ, UK

20. Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, China

21. Institute of Space Sciences (ICE, CSIC) , Campus UAB, Carrer de Can Magrans s/n, E-08193 Barcelona, Spain

22. School of Physics, O’Brien Centre for Science North, University College Dublin , Belfield, Dublin 4, Dublin, Ireland

23. Department of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USA

24. Turku Collegium for Science, Medicine and Technology, University of Turku , FI-20014 Turku, Finland

25. National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, China

26. School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 101408, China

27. Beijing Planetarium, Beijing Academy of Science and Technology , Beijing 100044, China

28. Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, China

29. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, China

Abstract

ABSTRACT We present the analysis of SN 2020wnt, an unusual hydrogen-poor superluminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterized by an early bump lasting ∼5 d, followed by a bright main peak. The SN reaches a peak absolute magnitude of M$_{r}^{\rm max}=-20.52\pm 0.03$ mag at ∼77.5 d 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 M⊙ and a pre-SN radius of 15 R⊙ that experiences a very energetic explosion of 45 × 1051 erg, producing 4 M⊙ 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.

Funder

UNRN

ANID

Finnish Academy of Science and Letters

MIUR

MICINN

FEDER

Royal Society

Science Foundation Ireland

Magnus Ehrnrooth Foundation

University of Hawaii

National Aeronautics and Space Administration