A radio-detected type Ia supernova with helium-rich circumstellar material.

Autor: Kool EC; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden. erik.kool@astro.su.se., Johansson J; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.; The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden., Sollerman J; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden., Moldón J; Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain.; Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, UK., Moriya TJ; National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Japan.; School of Physics and Astronomy, Faculty of Science, Monash University, Clayton, Victoria, Australia., Mattila S; Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Turku, Finland.; School of Sciences, European University Cyprus, Nicosia, Cyprus., Schulze S; The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden., Chomiuk L; Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA., Pérez-Torres M; Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain.; Facultad de Ciencias, Universidad de Zaragoza, Zaragoza, Spain., Harris C; Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA., Lundqvist P; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden., Graham M; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA., Yang S; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.; Henan Academy of Sciences, Zhengzhou, China., Perley DA; Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK., Strotjohann NL; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel., Fremling C; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA., Gal-Yam A; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel., Lezmy J; Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France., Maguire K; School of Physics, Trinity College Dublin, The University of Dublin, Dublin, Ireland., Omand C; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden., Smith M; Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France.; School of Physics and Astronomy, University of Southampton, Southampton, UK., Andreoni I; Joint Space-Science Institute, University of Maryland, College Park, MD, USA.; Department of Astronomy, University of Maryland, College Park, MD, USA.; Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA., Bellm EC; DIRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA., Bloom JS; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.; Lawrence Berkeley National Laboratory, Berkeley, CA, USA., De K; Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA., Groom SL; Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA., Kasliwal MM; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA., Masci FJ; Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA., Medford MS; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.; Lawrence Berkeley National Laboratory, Berkeley, CA, USA., Park S; Ulsan National Institute of Science and Technology, Ulsan, South Korea., Purdum J; Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA., Reynolds TM; The Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark., Riddle R; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA., Robert E; Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France., Ryder SD; School of Mathematical and Physical Sciences, Macquarie University, Sydney, New South Wales, Australia.; Astronomy, Astrophysics and Astrophotonics Research Centre, Macquarie University, Sydney, New South Wales, Australia., Sharma Y; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA., Stern D; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.
Jazyk: angličtina
Zdroj: Nature [Nature] 2023 May; Vol. 617 (7961), pp. 477-482. Date of Electronic Publication: 2023 May 17.
DOI: 10.1038/s41586-023-05916-w
Abstrakt: Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf stars destabilized by mass accretion from a companion star 1 , but the nature of their progenitors remains poorly understood. A way to discriminate between progenitor systems is through radio observations; a non-degenerate companion star is expected to lose material through winds 2 or binary interaction 3 before explosion, and the supernova ejecta crashing into this nearby circumstellar material should result in radio synchrotron emission. However, despite extensive efforts, no type Ia supernova (SN Ia) has ever been detected at radio wavelengths, which suggests a clean environment and a companion star that is itself a degenerate white dwarf star 4,5 . Here we report on the study of SN 2020eyj, a SN Ia showing helium-rich circumstellar material, as demonstrated by its spectral features, infrared emission and, for the first time in a SN Ia to our knowledge, a radio counterpart. On the basis of our modelling, we conclude that the circumstellar material probably originates from a single-degenerate binary system in which a white dwarf accretes material from a helium donor star, an often proposed formation channel for SNe Ia (refs.  6,7 ). We describe how comprehensive radio follow-up of SN 2020eyj-like SNe Ia can improve the constraints on their progenitor systems.
(© 2023. The Author(s).)
Databáze: MEDLINE
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