中国科学:物理学 力学 天文学(英文版)2024，Vol.67Issue(1) ：160-172.DOI:10.1007/s11433-023-2267-0

The dusty and extremely red progenitor of the type Ⅱ supernova 2023ixf in Messier 101

Danfeng Xiang Jun Mo Lingzhi Wang Xiaofeng Wang Jujia Zhang Han Lin Lifan Wang
中国科学:物理学 力学 天文学(英文版)2024，Vol.67Issue(1) ：160-172.DOI:10.1007/s11433-023-2267-0
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The dusty and extremely red progenitor of the type Ⅱ supernova 2023ixf in Messier 101

Danfeng Xiang 1Jun Mo 1Lingzhi Wang 2Xiaofeng Wang 3Jujia Zhang 4Han Lin 5Lifan Wang6
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作者信息

  • 1. Department of Physics,Tsinghua University,Beijing 100084,China
  • 2. South America Center for Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China
  • 3. Department of Physics,Tsinghua University,Beijing 100084,China;Beijing Planetarium,Beijing Academy of Sciences and Technology,Beijing 100044,China
  • 4. Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China;Key Laboratory for the Structure and Evolution of Celestial Objects,Chinese Academy of Sciences,Kunming 650216,China;International Centre of Supemovae,Yunnan Key Laboratory,Kunming 650216,China
  • 5. Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China;Key Laboratory for the Structure and Evolution of Celestial Objects,Chinese Academy of Sciences,Kunming 650216,China
  • 6. Mitchell Institute for Fundamental Physics and Astronomy,Texas A&M University College Station,TX 77843,USA
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Abstract

Stars with initial masses in the range of 8-25 solar masses are thought to end their lives as hydrogen-rich supernovae(SNe Ⅱ).Based on the pre-explosion images of Hubble space telescope(HST)and Spitzer space telescope,we place tight constraints on the progenitor candidate of type ⅡP SN 2023ixf in Messier 101.Fitting of the spectral energy distribution(SED)of its progenitor with dusty stellar spectral models results in an estimation of the effective temperature as 3091-258+422 K.The luminosity is estimated as lg(L/L⊙)～4.83,consistent with a red supergiant(RSG)star with an initial mass of 12-1+2M⊙.The derived mass loss rate(6×10-6-9×10-6 M⊙ yr-1)is much lower than that inferred from the flash spectroscopy of the SN,suggesting that the progenitor experienced a sudden increase in mass loss when approaching the final explosion.In the infrared bands,significant deviation from the range of regular RSGs in the color-magnitude diagram and period-luminosity space of the progenitor star indicates enhanced mass loss and dust formation.Combined with new evidence of polarization at the early phases of SN 2023ixf,such a violent mass loss is likely a result of binary interaction.

Key words

stellar evolution/mass loss/red supergiants/infrared emission/supernovae

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基金项目

National Natural Science Foundation of China(12288102)

National Natural Science Foundation of China(12033003)

National Natural Science Foundation of China(11633002)

Ma Huateng Foundation,the Scholar Program of Beijing Academy of Science and Technology(BS202002)

Tencent Xplorer Prize()

Chinese Academy of Sciences(CAS)()

CAS South America Center for Astronomy(CASSACA)in Santiago,Chile()

CAS()

People's Government of Yunnan Province()

YNAO()

Center for Astronomical Mega-Science,CAS()

出版年

2024
中国科学:物理学 力学 天文学(英文版)
中国科学院

中国科学:物理学 力学 天文学(英文版)

CSTPCD
影响因子：0.91
ISSN：1674-7348
参考文献量105
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