NAOC Open IR
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,Jujia8,9,10; 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
2021-03-01
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume909Issue:2
AbstractAbstract 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 ?19.12 ± 0.11 mag and a postpeak decline rate Δm 15(B) = 1.02 ± 0.07 mag. According to the quasi-bolometric light curve, we derive a peak luminosity of 1.25 × 1043 erg s?1 and a 56Ni mass of 0.63 ± 0.02 M ⊙. 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 ~130 ± 7 km s?1 day?1. Moreover, its early spectra (t < ? 7.9 days) show a prominent C ii λ6580 absorption feature, which disappeared in near-maximum-light spectra but reemerged at phases from t ~ + 8.7 days to t ~ + 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 λ6580-to-Si ii λ6355 velocity ratio (~0.81) observed in SN 2017hpa. The O i λ7774 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.
KeywordSupernovae Type Ia supernovae
DOI10.3847/1538-4357/abdeb9
Language英语
WOS IDIOP:0004-637X-909-2-abdeb9
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/58073
Collection中国科学院国家天文台
Affiliation1.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, People’s Republic of China; aliyi@xao.ac.cn
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 wang_xf@mail.tsinghua.edu.cn
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]. The Astrophysical Journal,2021,909(2).
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.The Astrophysical Journal,909(2).
MLA Zeng,Xiangyun,et al."SN 2017hpa: A Nearby Carbon-rich Type Ia Supernova with a Large Velocity Gradient".The Astrophysical Journal 909.2(2021).
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