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SN 2017hpa: A Nearby Carbon-rich Type Ia Supernova with a Large Velocity Gradient
Zeng, Xiangyun1,2; Wang, Xiaofeng3,4; Esamdin, Ali1; Pellegrino, Craig5,6; Zheng, WeiKang7; Zhang JJ(张居甲)8,9,10; Mo, Jun3; Li, Wenxiong3,11; Howell, D. Andrew5,6; Filippenko, Alexei V.7,12; Lin, Han3; Brink, Thomas G.7; Baron, Edward A.13; Burke, Jamison5,6; DerKacy, James M.13; McCully, Curtis5,6; Hiramatsu, Daichi5,6; Hosseinzadeh, Griffin5,14,15; Jeffers, Benjamin T.7; Ross, Timothy W.7; Stahl, Benjamin E.7,16; Stegman, Samantha7,17; Valenti, Stefano18; Wang, Lifan19; Xiang, Danfeng3; Zhang, Jicheng3; Zhang, Tianmeng20
Source PublicationASTROPHYSICAL JOURNAL
2021-03-01
Volume909Issue:2Pages:19
DOI10.3847/1538-4357/abdeb9
Contribution Rank第8完成单位
Indexed BySCI
KeywordSupernovae Type Ia supernovae
Abstract

We present extensive, well-sampled optical and ultraviolet photometry and optical spectra of the Type Ia supernova (SN Ia) 2017hpa. The light curves indicate that SN 2017hpa is a normal SN Ia with an absolute peak magnitude of M-max(B) approximate to -19.12 +/- 0.11 mag and a postpeak decline rate Delta m(15)(B) = 1.02 +/- 0.07 mag. According to the quasi-bolometric light curve, we derive a peak luminosity of 1.25 x 10(43) erg s(-1) and a Ni-56 mass of 0.63 +/- 0.02M(circle dot). The spectral evolution of SN 2017hpa is similar to that of normal Ia supernovae (SNe Ia), while it exhibits an unusually rapid velocity evolution resembling that of SN 1991bg-like SNe Ia or the high-velocity subclass of SNe Ia, with a postpeak velocity gradient of similar to 130 +/- 7 km s(-1) day(-1). Moreover, its early spectra (t < - 7.9 days) show a prominent C II lambda 6580 absorption feature, which disappeared in near-maximum-light spectra but reemerged at phases from t similar to + 8.7 days to t similar to + 11.7 days after maximum light. This implies that some unburned carbon may mix deep into the inner layer and is supported by the low C II lambda 6580-to-Si II lambda 6355 velocity ratio (similar to 0.81) observed in SN 2017hpa. The O I lambda 7774 line shows a velocity distribution like that of carbon. The prominent carbon feature, the low velocity seen in carbon and oxygen, and the large velocity gradient make SN 2017hpa stand out from other normal SNe Ia and are more consistent with predictions from a violent merger of two white dwarfs. Detailed modeling is still needed to reveal the nature of SN 2017hpa.

Funding ProjectNational Natural Science Foundation of China (NSFC)[11873081] ; National Natural Science Foundation of China (NSFC)[U2031209] ; National Natural Science Foundation of China (NSFC)[12033002] ; 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] ; High Level Talent-Heaven Lake Program of Xinjiang Uygur Autonomous Region of China ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; National Natural Science Foundation of China[11773067] ; National Natural Science Foundation of China[11403096] ; Youth Innovation Promotion Association of the CAS[2018081] ; Ten Thousand Talents Program of Yunnan for Top-notch Young Talents ; TABASGO Foundation ; Christopher R. Redlich Fund ; Miller Institute for Basic Research in Science (U.C. Berkeley) ; NSF[AST-1911225] ; NASA's Astrophysics Data Analysis Program[NNX13AF35G]
Funding OrganizationNational Natural Science Foundation of China (NSFC)[11873081, U2031209, 12033002, 11633002, 11761141001] ; 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 Beijing Academy of Science and Technology[DZ:BS202002] ; Chinese Academy of Sciences ; People's Government of Yunnan Province ; National Natural Science Foundation of China[11773067, 11403096] ; Youth Innovation Promotion Association of the CAS[2018081] ; Ten Thousand Talents Program of Yunnan for Top-notch Young Talents ; TABASGO Foundation ; Christopher R. Redlich Fund ; Miller Institute for Basic Research in Science (U.C. Berkeley) ; NSF[AST-1911225] ; NASA's Astrophysics Data Analysis Program[NNX13AF35G]
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:000629537600001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordDELAYED-DETONATION MODELS ; HUBBLE-SPACE-TELESCOPE ; CIRCUMSTELLAR MATERIAL ; OPTICAL-SPECTRA ; LIGHT CURVES ; FACTORY OBSERVATIONS ; DATA RELEASE ; PROGRAM ; ULTRAVIOLET ; EXPLOSION
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24262
Collection南方基地
中国科学院天体结构与演化重点实验室
Corresponding AuthorZeng, Xiangyun
Affiliation1.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, People's Republic of China
2.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China
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.Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216, People's Republic of China
9.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
10.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China
11.The School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
12.Miller Senior Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA
13.Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, USA
14.Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA
15.Las Cumbres Observatory, 6740 Cortona Drive Suite 102, Goleta, CA 9311-5575, USA
16.Department of Physics, University of California, Berkeley, CA 94720-7300, USA
17.Department of Chemistry, University of Wisconsin, Madison, WI 53706, USA
18.Department of Physics, University of California, Davis, CA 95616, USA
19.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
20.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China
Recommended Citation
GB/T 7714
Zeng, Xiangyun,Wang, Xiaofeng,Esamdin, Ali,et al. SN 2017hpa: A Nearby Carbon-rich Type Ia Supernova with a Large Velocity Gradient[J]. ASTROPHYSICAL JOURNAL,2021,909(2):19.
APA Zeng, Xiangyun.,Wang, Xiaofeng.,Esamdin, Ali.,Pellegrino, Craig.,Zheng, WeiKang.,...&Zhang, Tianmeng.(2021).SN 2017hpa: A Nearby Carbon-rich Type Ia Supernova with a Large Velocity Gradient.ASTROPHYSICAL JOURNAL,909(2),19.
MLA Zeng, Xiangyun,et al."SN 2017hpa: A Nearby Carbon-rich Type Ia Supernova with a Large Velocity Gradient".ASTROPHYSICAL JOURNAL 909.2(2021):19.
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