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Probing the final-stage progenitor evolution for Type IIP Supernova 2017eaw in NGC 6946
Rui, Liming1,2; Wang, Xiaofeng1,2; Mo, Jun1,2; Xiang, Danfeng1,2; Zhang JJ(张居甲)2,3; Maund, Justyn R.4; Gal-Yam, Avishy5; Wang, Lifan6; Zhang, Tianmeng7
发表期刊MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2019-05-01
卷号485期号:2页码:1990-2000
DOI10.1093/mnras/stz503
产权排序第2完成单位
收录类别SCI ; EI
关键词stars: evolution supernovae: general supernovae: individual: SN 2017eaw galaxies: individual: NGC 6946
摘要

We presented a detailed analysis of progenitor properties of type IIP supernova 2017eaw in NGC 6946, based on the pre-explosion images and early-time observations obtained immediately after the explosion. An unusually red star, with M-F814W =-6.9 mag and mF606W -m(F814W) = 2.9 +/- 0.2 mag, can be identified at the SN position in the pre-discovery Hubble Space Telescope (HST) images taken in 2016. The observed spectral energy distribution of this star, covering the wavelength of 0.6-2.0 mu m, matches that of an M4-type red supergiant (RSG) with a temperature of about 3550 K. These results suggest that SN 2017eaw has a RSG progenitor with an initial mass of 12 +/- 2 M-circle dot. The absolute F814W-band magnitude of this progenitor star is found to evolve from -7.2 mag in 2004 to -6.9 mag in 2016. Such a dimming effect is, however, unpredicted for an RSG in its neon/oxygen burning phase when its luminosity should modestly increase. The spectrum of SN 2017eaw taken a few hours after discovery clearly shows a narrow H-alpha emission feature blueshifted by similar to 160 km s(-1). This narrow component disappeared in the spectrum taken two days later, suggesting the presence of a circumstellar material (CSM) shell (i.e. at a distance of < 2.1-4.3 x 10(14) cm). Combining the inferred distance with the expansion velocity of the CSM, we suggest that the progenitor of SN 2017eaw should have experienced violent mass-loss at about 1-2 yr prior to explosion, perhaps invoked by pulsational envelop ejection. This mechanism may help explain its luminosity decline in 2016 as well as the lack of detections of RSGs with relatively higher initial mass as progenitors of SNe IIP.

资助项目National Natural Science Foundation of China (NSFC)[11325313] ; National Natural Science Foundation of China (NSFC)[11633002] ; National Natural Science Foundation of China (NSFC)[11761141001] ; National Program on Key Research and Development Project[2016YFA0400803] ; NSFC[11203034] ; NSFC[11403096] ; NSFC[11773067] ; Youth Innovation Promotion Association of the CAS[2018081] ; Western Light Youth Project ; Key Research Program of the CAS[KJZD-EW-M06] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; Royal Society University Research Fellowship
项目资助者National Natural Science Foundation of China (NSFC)[11325313, 11633002, 11761141001] ; National Program on Key Research and Development Project[2016YFA0400803] ; NSFC[11203034, 11403096, 11773067] ; Youth Innovation Promotion Association of the CAS[2018081] ; Western Light Youth Project ; Key Research Program of the CAS[KJZD-EW-M06] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; Royal Society University Research Fellowship
语种英语
学科领域天文学 ; 恒星与银河系 ; 恒星形成与演化
学科门类理学 ; 理学::天文学
文章类型Article
出版者OXFORD UNIV PRESS
出版地GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
WOS记录号WOS:000474886200036
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]RED SUPERGIANTS ; SHOCK BREAKOUT ; MASSIVE STARS ; P SUPERNOVA ; RISE ; COOL
EI入藏号20221612004103
EI主题词Supernovae
EI分类号657.2 Extraterrestrial Physics and Stellar Phenomena
引用统计
被引频次:31[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/20561
专题南方基地
中国科学院天体结构与演化重点实验室
通讯作者Rui, Liming; Wang, Xiaofeng
作者单位1.Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China
2.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
3.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
4.Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK
5.Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel
6.Physics and Astronomy Department, Texas A&M University, College Station, TX 77843, USA
7.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
第一作者单位中国科学院云南天文台
通讯作者单位中国科学院云南天文台
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Rui, Liming,Wang, Xiaofeng,Mo, Jun,et al. Probing the final-stage progenitor evolution for Type IIP Supernova 2017eaw in NGC 6946[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2019,485(2):1990-2000.
APA Rui, Liming.,Wang, Xiaofeng.,Mo, Jun.,Xiang, Danfeng.,Zhang JJ.,...&Zhang, Tianmeng.(2019).Probing the final-stage progenitor evolution for Type IIP Supernova 2017eaw in NGC 6946.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,485(2),1990-2000.
MLA Rui, Liming,et al."Probing the final-stage progenitor evolution for Type IIP Supernova 2017eaw in NGC 6946".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 485.2(2019):1990-2000.
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