The dusty and extremely red progenitor of the typeⅡsupernova 2023ixf in Messier 101  

作　　者：Danfeng Xiang Jun Mo Lingzhi Wang Xiaofeng Wang Jujia Zhang Han Lin Lifan Wang 

机构地区：[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]Beijing Planetarium,Beijing Academy of Sciences and Technology,Beijing 100044,China [4]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [5]Key Laboratory for the Structure and Evolution of Celestial Objects,Chinese Academy of Sciences,Kunming 650216,China [6]International Centre of Supernovae,Yunnan Key Laboratory,Kunming 650216,China [7]Mitchell Institute for Fundamental Physics and Astronomy,Texas A&M University,College Station,TX 77843,USA

出　　处：《Science China(Physics,Mechanics & Astronomy)》2024年第1期160-172,共13页中国科学：物理学、力学、天文学（英文版）

基　　金：supported by the National Natural Science Foundation of China(Grant Nos.12288102,12033003,and 11633002);the Ma Huateng Foundation;the Scholar Program of Beijing Academy of Science and Technology(Grant No.DZ:BS202002);the Tencent Xplorer Prize;sponsored(in part)by the Chinese Academy of Sciences(CAS);through a grant to the CAS South America Center for Astronomy(CASSACA)in Santiago,Chile;Funding for the LJT has been provided by the CAS and the People’s Government of Yunnan Province。

摘　　要：Stars with initial masses in the range of 8-25 solar masses are thought to end their lives as hydrogen-rich supernovae(SNeⅡ).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+422-258K.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.

关 键 词：stellar evolution mass loss red supergiants infrared emission SUPERNOVAE 

分 类 号：P145.3[天文地球—天体物理]