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OPTICAL OBSERVATIONS OF THE TYPE IA SUPERNOVA SN 2011fe IN M101 FOR NEARLY 500 DAYS
Zhang, Kaicheng1; Wang, Xiaofeng1; Zhang JJ(张居甲)2,3; Zhang, Tianmeng4; Ganeshalingam, Mohan5; Li, Weidong5; Filippenko, Alexei V.5; Zhao, Xulin1; Zheng, Weikang5; Bai JM(白金明)2,3; Chen, Jia1; Chen, Juncheng1; Huang, Fang1,6; Mo, Jun1; Rui, Liming1; Song, Hao1; Sai, Hanna1; Li, Wenxiong1; Wang, Lifan7; Wu, Chao4
Source PublicationASTROPHYSICAL JOURNAL
2016-03-20
Volume820Issue:1
DOI10.3847/0004-637X/820/1/67
Contribution Rank第2完成单位
Indexed BySCI
KeywordSupernovae: General Supernovae: Individual (Sn 2011fe)
Abstract

We present well-sampled optical observations of the bright Type Ia supernova (SN Ia) SN 2011fe in M101. Our data, starting from similar to 16 days before maximum light and extending to similar to 463 days after maximum, provide an unprecedented time series of spectra and photometry for a normal SN Ia. Fitting the early-time rising light curve, we find that the luminosity evolution of SN 2011fe follows a t(n) law, with the index n being close to 2.0 in the VRI bands but slightly larger in the U and B bands. Combining the published ultraviolet (UV) and near-infrared (NIR) photometry, we derive the contribution of UV/NIR emission relative to the optical. SN 2011fe is found to have stronger UV emission and reaches its UV peak a few days earlier than other SNe Ia with similar Delta m(15)(B), suggestive of less trapping of high-energy photons in the ejecta. Moreover, the U-band light curve shows a notably faster decline at late phases (t approximate to 100-300 days), which also suggests that the ejecta may be relatively transparent to UV photons. These results favor the notion that SN 2011fe might have a progenitor system with relatively lower metallicity. On the other hand, the early-phase spectra exhibit prominent high-velocity features (HVFs) of O I lambda 7773 and the Ca II NIR triplet, but only barely detectable in Si II 6355. This difference can be caused by either an ionization/temperature effect or an abundance enhancement scenario for the formation of HVFs; it suggests that the photospheric temperature of SN 2011fe is intrinsically low, perhaps owing to incomplete burning during the explosion of the white dwarf.

Funding ProjectNational Science Foundation of China (NSFC)[11178003] ; National Science Foundation of China (NSFC)[11325313] ; National Science Foundation of China (NSFC)[11403096] ; National Science Foundation of China (NSFC)[11203034] ; Major State Basic Research Development Program[2013CB834903] ; Key Research Program of the Chinese Academy of Sciences[KJZD-EW-M06] ; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; NSF[AST-1211916] ; TABASGO Foundation ; People's Government of Yunnan Province ; Chinese Academy of Sciences ; Christopher R. Redlich Fund
Funding OrganizationNational Science Foundation of China (NSFC)[11178003, 11325313, 11403096, 11203034] ; Major State Basic Research Development Program[2013CB834903] ; Key Research Program of the Chinese Academy of Sciences[KJZD-EW-M06] ; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; NSF[AST-1211916] ; TABASGO Foundation ; People's Government of Yunnan Province ; Chinese Academy of Sciences ; Christopher R. Redlich Fund
Language英语
Subject Area天文学 ; 天体物理学 ; 实测天体物理学 ; 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:000372787000066
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordLIGHT CURVES ; RISE-TIME ; NEBULAR SPECTRA ; COMPANION STAR ; ULTRAVIOLET ; PROGENITOR ; TELESCOPE ; SPECTROSCOPY ; SYSTEM ; ENVIRONMENT
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9575
Collection丽江天文观测站(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, China
2.Yunnan Astronomical Observatory of China, Chinese Academy of Sciences, Kunming, 650011, China
3.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
4.National Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, 100012, China
5.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
6.Astronomy Department, Beijing Normal University, Beijing, 100875, China
7.Physics and Astronomy Department, Texas A&M University, College Station, TX 77843, USA
Recommended Citation
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Zhang, Kaicheng,Wang, Xiaofeng,Zhang JJ,et al. OPTICAL OBSERVATIONS OF THE TYPE IA SUPERNOVA SN 2011fe IN M101 FOR NEARLY 500 DAYS[J]. ASTROPHYSICAL JOURNAL,2016,820(1).
APA Zhang, Kaicheng.,Wang, Xiaofeng.,Zhang JJ.,Zhang, Tianmeng.,Ganeshalingam, Mohan.,...&Wu, Chao.(2016).OPTICAL OBSERVATIONS OF THE TYPE IA SUPERNOVA SN 2011fe IN M101 FOR NEARLY 500 DAYS.ASTROPHYSICAL JOURNAL,820(1).
MLA Zhang, Kaicheng,et al."OPTICAL OBSERVATIONS OF THE TYPE IA SUPERNOVA SN 2011fe IN M101 FOR NEARLY 500 DAYS".ASTROPHYSICAL JOURNAL 820.1(2016).
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