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SN 2017fgc: A Fast-expanding Type Ia Supernova Exploded in Massive Shell Galaxy NGC 474
Zeng, Xiangyun1,2; Wang, Xiaofeng3,4; Esamdin, Ali1; Pellegrino, Craig5,6; Burke, Jamison5,6; Stahl, Benjamin E.7,8; Zheng, WeiKang7; Filippenko, Alexei V.7,9; Howell, D. Andrew5,6; Sand, D. J.10; Valenti, Stefano11; Mo, Jun3; Xi, Gaobo3; Liu, Jialian3; Zhang JJ(张居甲)12,13,14; Li, Wenxiong15; Iskandar, Abdusamatjan1,2; Zhang, Mengfan1; Lin, Han3; Sai, Hanna3; Xiang, Danfeng3; Wei, Peng1; Zhang, Tianmeng16; Reichart, D. E.17; Brink, Thomas G.7; McCully, Curtis5,6; Hiramatsu, Daichi5,6; Hosseinzadeh, Griffin5,6,18; Jeffers, Benjamin T.7; Ross, Timothy W.7; Stegman, Samantha7,19; Wang, Lifan20; Zhang, Jicheng3; Ma, Shuo1,2
Source PublicationASTROPHYSICAL JOURNAL
2021-09
Volume919Issue:1
DOI10.3847/1538-4357/ac0e9c
Contribution Rank第12完成单位
Indexed BySCI
Abstract

We present extensive optical photometric and spectroscopic observations of the high-velocity (HV) Type Ia supernova (SN Ia) 2017fgc, covering the phase from similar to 12 days before to similar to 389 days after maximum brightness. SN 2017fgc is similar to normal SNe Ia, with an absolute peak magnitude of M-max(B) approximate to -19.32 +/- 0.13 mag and a post-peak decline of Delta m(15)(B) = 1.05 +/- 0.07 mag. Its peak bolometric luminosity is derived as (1.32 +/- 0.13) x 10(43) erg s(-1), corresponding to a Ni-56 mass of 0.51 +/- 0.03 M-circle dot. The light curves of SN 2017fgc are found to exhibit excess emission in the UBV bands in the early nebular phase and pronounced secondary shoulder/maximum features in the RrIi bands. Its spectral evolution is similar to that of HV SNe Ia, with a maximum-light Si II velocity of 15,000 +/- 150 km s(-1) and a post-peak velocity gradient of similar to 120 +/- 10 km s(-1) day(-1). The Fe II and Mg II lines blended near 4300 angstrom and the Fe II, Si II, and Fe III lines blended near 4800 angstrom are obviously stronger than those of normal SNe Ia. Inspecting a large sample reveals that the strength of the two blends in the spectra, and the secondary peak in the i/r-band light curves, are found to be positively correlated with the maximum-light Si II velocity. Such correlations indicate that HV SNe Ia may experience more complete burning in the ejecta and/or that their progenitors have higher metallicity. Examining the birthplace environment of SN 2017fgc suggests that it likely arose from a stellar environment with young and high-metallicity populations.

Funding ProjectNational Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11873081] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[U2031209] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033002] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11633002] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11803076] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11761141001] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11773067] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11403096] ; National Program on Key Research and Development Project[2016YFA0400803] ; High Level Talent-Heaven Lake Program of Xinjiang Uygur Autonomous Region of China ; Scholar Program of the Beijing Academy of Science and Technology[DZ:BS202002] ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; Youth Innovation Promotion Association of the CAS[2018081] ; Ten Thousand Talents Program of Yunnan for Topnotch Young Talents ; TABASGO Foundation ; Christopher R. Redlich Fund ; Miller Institute for Basic Research in Science ; U.S. National Science Foundation (NSF)National Science Foundation (NSF)[AST-1821967] ; U.S. National Science Foundation (NSF)National Science Foundation (NSF)[1821987] ; U.S. National Science Foundation (NSF)National Science Foundation (NSF)[1813708] ; U.S. National Science Foundation (NSF)National Science Foundation (NSF)[1813466] ; U.S. National Science Foundation (NSF)National Science Foundation (NSF)[1908972] ; Heising-Simons Foundation[2020-1864] ; NSFNational Science Foundation (NSF)[AST-1911225]
Funding OrganizationNational Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11873081, U2031209, 12033002, 11633002, 11803076, 11761141001, 11773067, 11403096] ; National Program on Key Research and Development Project[2016YFA0400803] ; High Level Talent-Heaven Lake Program of Xinjiang Uygur Autonomous Region of China ; Scholar Program of the Beijing Academy of Science and Technology[DZ:BS202002] ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; Youth Innovation Promotion Association of the CAS[2018081] ; Ten Thousand Talents Program of Yunnan for Topnotch Young Talents ; TABASGO Foundation ; Christopher R. Redlich Fund ; Miller Institute for Basic Research in Science ; U.S. National Science Foundation (NSF)National Science Foundation (NSF)[AST-1821967, 1821987, 1813708, 1813466, 1908972] ; Heising-Simons Foundation[2020-1864] ; NSFNational Science Foundation (NSF)[AST-1911225]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星形成与演化
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:000697836000001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordDELAYED-DETONATION MODEL ; LIGHT CURVES ; FOLLOW-UP ; INFRARED OBSERVATIONS ; CIRCUMSTELLAR MATTER ; SPECTRAL EVOLUTION ; OPTICAL-SPECTRA ; DATA RELEASE ; RISE-TIME ; PROGRAM
Citation statistics
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24573
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.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, People's Republic of China; wang_xf@mail.tsinghua.edu.cn;
2.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China; aliyi@xao.ac.cn;
3.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, People's Republic of China;
4.Beijing Planetarium, Beijing Academy of Science of Technology, Beijing 100044, People's Republic of China;
5.Department of Physics, University of California, Santa Barbara, CA 93106-9530, USA;
6.Las Cumbres Observatory, 6740 Cortona Drive Suite 102, Goleta, CA 93117-5575, USA;
7.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA;
8.Department of Physics, University of California, Berkeley, CA 94720-7300, USA;
9.Miller Senior Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA;
10.Steward Observatory, University of Arizona, 933 North Cherry Avenue, Rm. N204, Tucson, AZ 85721-0065, USA;
11.Department of Physics, University of California, Davis, CA 95616, USA;
12.Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
13.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
14.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China;
15.The School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel;
16.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China;
17.Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA;
18.Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA;
19.Department of Chemistry, University of Wisconsin, Madison, WI 53706, USA;
20.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
Recommended Citation
GB/T 7714
Zeng, Xiangyun,Wang, Xiaofeng,Esamdin, Ali,et al. SN 2017fgc: A Fast-expanding Type Ia Supernova Exploded in Massive Shell Galaxy NGC 474[J]. ASTROPHYSICAL JOURNAL,2021,919(1).
APA Zeng, Xiangyun.,Wang, Xiaofeng.,Esamdin, Ali.,Pellegrino, Craig.,Burke, Jamison.,...&Ma, Shuo.(2021).SN 2017fgc: A Fast-expanding Type Ia Supernova Exploded in Massive Shell Galaxy NGC 474.ASTROPHYSICAL JOURNAL,919(1).
MLA Zeng, Xiangyun,et al."SN 2017fgc: A Fast-expanding Type Ia Supernova Exploded in Massive Shell Galaxy NGC 474".ASTROPHYSICAL JOURNAL 919.1(2021).
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