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Observations of SN 2017ein Reveal Shock Breakout Emission and a Massive Progenitor Star for a Type Ic Supernova
Xiang, Danfeng1; Wang, Xiaofeng1; Mo, Jun1; Wang, Lingjun2; Smartt, Stephen3; Fraser, Morgan4; Ehgamberdiev, Shuhrat A.5; Mirzaqulov, Davron5; Zhang JJ(张居甲)6,7,8; Zhang, Tianmeng9; Vinko, Jozsef10,11,12; Wheeler, J. Craig12; Hosseinzadeh, Griffin13,14; Howell, D. Andrew13,14; McCully, Curtis13; DerKacy, James M.14; Baron, E.14; Brown, Peter16; Zhang, Xianfei17; Bi, Shaolan17; Song, Hao1; Zhang, Kaicheng1; Rest, A.18,19; Nomoto, Ken'ichi20; Tolstov, Alexey20,23; Blinnikov, Sergei20,21,22
Source PublicationASTROPHYSICAL JOURNAL
2019-02-01
Volume871Issue:2Pages:20
DOI10.3847/1538-4357/aaf8b0
Contribution Rank第6完成单位
Indexed BySCI
Keywordsupernovae: general supernovae: individual (SN 2017ein) stars: Wolf-Rayet
Abstract

We present optical and ultraviolet observations of nearby Type Ic supernova (SN Ic) SN 2017ein, as well as a detailed analysis of its progenitor properties from both the early-time observations and the prediscovery Hubble Space Telescope (HST) images. The optical light curves started from within 1 day to similar to 275 days after explosion, and optical spectra range from similar to 2 days to similar to 90 days after explosion. Compared to other normal SNe Ic like SN 2007gr and SN 2013ge, SN 2017ein seems to have more prominent C II absorption and higher expansion velocities in early phases, suggestive of relatively lower ejecta mass. The earliest photometry obtained for SN 2017ein shows indications of shock cooling. The best fit obtained by including a shock-cooling component gives an estimate of the envelope mass as similar to 0.02 M-circle dot and stellar radius as 8 +/- 4 R-circle dot. Examining the pre-explosion images taken with the HST WFPC2, we find that the SN position coincides with a luminous and blue point-like source, with an extinction-corrected absolute magnitude of M-V similar to -8.2 mag and M-I similar to -7.7 mag. Comparisons of the observations to the theoretical models indicate that the counterpart source was either a single W-R star or a binary whose members had high initial masses, or a young compact star cluster. To further distinguish between different scenarios requires revisiting the site of the progenitor with HST after the SN fades away.

Funding ProjectNational Natural Science Foundation of China (NSFC)[11178003] ; National Natural Science Foundation of China (NSFC)[11325313] ; National Natural Science Foundation of China (NSFC)[11633002] ; National Program on Key Research and Development Project[2016YFA0400803] ; NSFC[11403096] ; NSFC[11773067] ; NSFC[11203034] ; Key Research Program of the CAS[KJZD-EW-M06] ; Youth Innovation Promotion Association of the CAS[2018081] ; CAS "Light of West China" Program ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; NASA under the Near Earth Objects Observations program (NEOO)[NN12AR55G] ; National Program on Key Research and Development Project of China[2016YFA0400801] ; US National Science Foundation (NSF)[AST-1313484] ; NASA[NNX16AB256] ; Royal Society Science Foundation Ireland University Research Fellowship ; project "Transient Astrophysical Objects" of the National Research, Development and Innovation Office (NKFIH), Hungary - European Union[GINOP 2.3.2-15-2016-00033] ; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan ; JSPS[JP16K17658] ; JSPS[JP26400222] ; JSPS[JP16H02168] ; JSPS[JP17K05382] ; JSPS[JP16H02166] ; [RSF 18-12-00522]
Funding OrganizationNational Natural Science Foundation of China (NSFC)[11178003, 11325313, 11633002] ; National Program on Key Research and Development Project[2016YFA0400803] ; NSFC[11403096, 11773067, 11203034] ; Key Research Program of the CAS[KJZD-EW-M06] ; Youth Innovation Promotion Association of the CAS[2018081] ; CAS "Light of West China" Program ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; NASA under the Near Earth Objects Observations program (NEOO)[NN12AR55G] ; National Program on Key Research and Development Project of China[2016YFA0400801] ; US National Science Foundation (NSF)[AST-1313484] ; NASA[NNX16AB256] ; Royal Society Science Foundation Ireland University Research Fellowship ; project "Transient Astrophysical Objects" of the National Research, Development and Innovation Office (NKFIH), Hungary - European Union[GINOP 2.3.2-15-2016-00033] ; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan ; JSPS[JP16K17658, JP26400222, JP16H02168, JP17K05382, JP16H02166] ; [RSF 18-12-00522]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星天文学
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:000457281200009
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordGAMMA-RAY BURST ; LIGHT CURVES ; EVOLUTION ; IB ; CONSTRAINTS ; POPULATIONS ; PHOTOMETRY ; GRB-060218 ; HELIUM ; MODELS
Citation statistics
Cited Times:8[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/19332
Collection南方基地
中国科学院天体结构与演化重点实验室
Corresponding AuthorXiang, Danfeng
Affiliation1.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People's Republic of China
2.Astroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People's Republic of China
3.Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK
4.School of Physics, University College Dublin, Belfield, Dublin 4, Ireland
5.Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Uzbekistan, Tashkent, 100052, Uzbekistan
6.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
7.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
8.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China
9.National Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, 100012, People's Republic of China
10.Konkoly Observatory, MTA CSFK, Konkoly Thege M. ut 15-17, Budapest, 1121, Hungary
11.Department of Optics & Quantum Electronics, University of Szeged, Dom ter 9, Szeged, 6720 Hungary
12.Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
13.Las Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA
14.Department of Physics, University of California, Santa Barbara, CA 93106-9530, USA
15.Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA
16.George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy, Texas A. & M. University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843, USA
17.Department of Astronomy, Beijing Normal University, Beijing 100875, People's Republic of China
18.Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
19.Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA
20.Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
21.Institute for Theoretical and Experimental Physics (ITEP), 117218, Moscow, Russia
22.All-Russia Research Institute of Automatics (VNIIA), 127055, Moscow, Russia
23.The Open University of Japan, 2-11, Wakaba, Mihama-ku, Chiba, Chiba 261-8586, Japan
Recommended Citation
GB/T 7714
Xiang, Danfeng,Wang, Xiaofeng,Mo, Jun,et al. Observations of SN 2017ein Reveal Shock Breakout Emission and a Massive Progenitor Star for a Type Ic Supernova[J]. ASTROPHYSICAL JOURNAL,2019,871(2):20.
APA Xiang, Danfeng.,Wang, Xiaofeng.,Mo, Jun.,Wang, Lingjun.,Smartt, Stephen.,...&Blinnikov, Sergei.(2019).Observations of SN 2017ein Reveal Shock Breakout Emission and a Massive Progenitor Star for a Type Ic Supernova.ASTROPHYSICAL JOURNAL,871(2),20.
MLA Xiang, Danfeng,et al."Observations of SN 2017ein Reveal Shock Breakout Emission and a Massive Progenitor Star for a Type Ic Supernova".ASTROPHYSICAL JOURNAL 871.2(2019):20.
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