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

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A radio-detected type Ia supernova with helium-rich circumstellar material
Nature ( IF 50.5 ) Pub Date : 2023-05-17 , DOI: 10.1038/s41586-023-05916-w
Erik C Kool ₁ , Joel Johansson _{1,

2} , Jesper Sollerman ₁ , Javier Moldón _{3,

4} , Takashi J Moriya _{5,

6} , Seppo Mattila _{7,

8} , Steve Schulze ₂ , Laura Chomiuk ₉ , Miguel Pérez-Torres _{3,

10} , Chelsea Harris ₉ , Peter Lundqvist ₁ , Matthew Graham ₁₁ , Sheng Yang _{1,

12} , Daniel A Perley ₁₃ , Nora Linn Strotjohann ₁₄ , Christoffer Fremling ₁₁ , Avishay Gal-Yam ₁₄ , Jeremy Lezmy ₁₅ , Kate Maguire ₁₆ , Conor Omand ₁ , Mathew Smith _{15,

17} , Igor Andreoni _{18,

19,

20} , Eric C Bellm ₂₁ , Joshua S Bloom _{22,

23} , Kishalay De ₂₄ , Steven L Groom ₂₅ , Mansi M Kasliwal ₁₁ , Frank J Masci ₂₅ , Michael S Medford _{22,

23} , Sungmin Park ₂₆ , Josiah Purdum ₂₇ , Thomas M Reynolds ₂₈ , Reed Riddle ₁₁ , Estelle Robert ₁₅ , Stuart D Ryder _{29,

30} , Yashvi Sharma ₁₁ , Daniel Stern ₃₁

Affiliation

The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.
The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden.
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.
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.
Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Turku, Finland.
School of Sciences, European University Cyprus, Nicosia, Cyprus.
Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA.
Facultad de Ciencias, Universidad de Zaragoza, Zaragoza, Spain.
Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
Henan Academy of Sciences, Zhengzhou, China.
Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK.
Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France.
School of Physics, Trinity College Dublin, The University of Dublin, Dublin, Ireland.
School of Physics and Astronomy, University of Southampton, Southampton, UK.
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.
DIRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA.
Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
Lawrence Berkeley National Laboratory, Berkeley, CA, USA.
Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA.
Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA.
Ulsan National Institute of Science and Technology, Ulsan, South Korea.
Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA.
The Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark.
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.
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.

Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf stars destabilized by mass accretion from a companion star¹, 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 winds² or binary interaction³ 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.

中文翻译：

射电探测到的 Ia 型超新星，具有富含氦的星周物质

Ia 型超新星 (SNe Ia) 是简并白矮星的热核爆炸，由于伴星的质量吸积而不稳定¹ ，但对其前身的性质仍然知之甚少。区分祖先系统的一种方法是通过无线电观测。预计非简并伴星在爆炸前会通过风²或双星相互作用³失去物质，超新星喷射物撞击附近的星周物质应会导致射电同步加速器发射。然而，尽管付出了巨大的努力，仍然没有在射电波长范围内检测到 Ia 型超新星 (SN Ia)，这表明存在清洁的环境和一颗伴星，该伴星本身就是一颗简并白矮星^4,5 。在这里，我们报告了 SN 2020eyj 的研究，SN 2020eyj 是一个 SN Ia，它显示出富含氦的星周物质，其光谱特征、红外发射以及据我们所知首次在 SN Ia 中出现了射电对应物。根据我们的模型，我们得出结论，星周物质可能起源于单简并双星系统，其中白矮星从氦供体星吸积物质，这是超新星 Ia 经常提出的形成通道（参考文献^6,7 ）。我们描述了类似 SN 2020eyj 的 SNe Ia 的全面无线电跟踪如何改善对其祖先系统的限制。

更新日期：2023-05-18

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