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ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin
Wang, Xiaofeng1,2; Lin, Weili1; Zhang JJ(张居甲)3,4; Zhang, Tianmeng5,6; Cai, Yongzhi1; Zhang, Kaicheng1; Filippenko, Alexei V.7,8; Graham, Melissa9; Maeda, Keiichi10; Mo, Jun1; Xiang, Danfeng1; Xi, Gaobo1; Yan, Shengyu1; Wang, Lifan11; Wang, Lingjun12; Kawabata, Koji13; Zhai Q(翟倩)3,4
Source PublicationASTROPHYSICAL JOURNAL
2021-08
Volume917Issue:2
DOI10.3847/1538-4357/ac0c17
Contribution Rank第3完成单位
Indexed BySCI
Abstract

ASASSN-14ms may represent the most luminous Type Ibn supernova (SN Ibn) ever detected, with an absolute U-band magnitude brighter than -22.0 mag and a total bolometric luminosity >1.0 x 10(44) erg s(-1) near maximum light. The early-time spectra of this SN are characterized by a blue continuum on which are superimposed narrow P Cygni profile lines of He i, suggesting the presence of slowly moving (similar to 1000 km s(-1)), He-rich circumstellar material (CSM). At 1-2 months after maximum brightness, the He i line profiles become only slightly broader, with blueshifted velocities of 2000-3000 km s(-1), consistent with the CSM shell being continuously accelerated by the SN light and ejecta. Like most SNe Ibn, the light curves of ASASSN-14ms show rapid post-peak evolution, dropping by similar to 7 mag in the V band over three months. Such a rapid post-peak decline and high luminosity can be explained by interaction between SN ejecta and helium-rich CSM of 0.9 M (circle dot) at a distance of similar to 10(15) cm. The CSM around ASASSN-14ms is estimated to originate from a pre-explosion event with a mass-loss rate of 6.7 M (circle dot) yr(-1) (assuming a velocity of similar to 1000 km s(-1)), which is consistent with abundant He-rich material violently ejected during the late Wolf-Rayet (WN9-11 or Opfe) stage. After examining the light curves for a sample of SNe Ibn, we find that the more luminous ones tend to have slower post-peak decline rates, reflecting that the observed differences may arise primarily from discrepancies in the CSM distribution around the massive progenitors.

Funding ProjectNational Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033003] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11633002] ; Major State Basic Research Development ProgramNational Basic Research Program of China[2016YFA0400803] ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; TABASGO Foundation ; Christopher R. Redlich Fund ; U.C. Berkeley Miller Institute for Basic Research in Science ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP18H05223] ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP20H00174] ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP20H04737] ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; W. M. Keck FoundationW.M. Keck Foundation
Funding OrganizationNational Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033003, 11633002] ; Major State Basic Research Development ProgramNational Basic Research Program of China[2016YFA0400803] ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; TABASGO Foundation ; Christopher R. Redlich Fund ; U.C. Berkeley Miller Institute for Basic Research in Science ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP18H05223, JP20H00174, JP20H04737] ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; W. M. Keck FoundationW.M. Keck Foundation
Language英语
Subject Area天文学 ; 恒星与银河系
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS IDWOS:000687842200001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordRICH CIRCUMSTELLAR MEDIUM ; WOLF-RAYET STAR ; MASSIVE STARS ; CORE-COLLAPSE ; LIGHT CURVES ; OPTICAL OBSERVATIONS ; SN 2009JF ; EVOLUTION ; TRANSIENT ; EMISSION
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24524
Collection南方基地
中国科学院天体结构与演化重点实验室
Corresponding AuthorWang, Xiaofeng
Affiliation1.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, People's Republic of China wang_xf@mail.tsinghua.edu.cn, linwl@mail.tsinghua.edu.cn;
2.Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, People's Republic of China;
3.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
4.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
5.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China;
6.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, People's Republic of China;
7.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA;
8.Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA;
9.Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA;
10.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan;
11.Physics and Astronomy Department, Texas A&M University, College Station, TX 77843, USA;
12.Astroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People's Republic of China;
13.Department of Physical Science, Hiroshima University, Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
Recommended Citation
GB/T 7714
Wang, Xiaofeng,Lin, Weili,Zhang JJ,et al. ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin[J]. ASTROPHYSICAL JOURNAL,2021,917(2).
APA Wang, Xiaofeng.,Lin, Weili.,Zhang JJ.,Zhang, Tianmeng.,Cai, Yongzhi.,...&Zhai Q.(2021).ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin.ASTROPHYSICAL JOURNAL,917(2).
MLA Wang, Xiaofeng,et al."ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin".ASTROPHYSICAL JOURNAL 917.2(2021).
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