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Detection of 2 MeV Spectral Bump and ∼40 MeV Emission Line from GRB 221009A

  • Authors: Zhi-Qiang Ding, Zhenxia Zhang, Yanqiu Zhang, Rui-Ze Shi, Xinqiao Li, Zhuo Li, Zhenghua An, Shaolin Xiong, Roberto Battiston, Shuangnan Zhang, Hua Feng, Dali Zhang, Yanbing Xu, Ping Wang, Xiaoyun Zhao, Yuqian Ma, Hong Lu, Xiangyang Wen, Yongjie Zhang, Xuhui Shen, Shigeng Yuan, Siquan Yang, Rongxue Kang, Chao Zheng, Yan Huang, Wen Su, Shengli Liu, Hui Wang, Xiaohua Liang, Jinzhou Wang, Ke Gong, Xiaojing Liu, Yaqing Liu, Sheng Yang, Zeren Zhima, Jianping Huang, Wei Chu, Na Zhou, Roberto Iuppa, Francesco Maria Follega, Marco Cristoforetti, Wangchen Xue, Lu Wang, Jiaqi Zheng, Jiacong Liu, Chenwei Wang, Wenjun Tan, Zhenghang Yu, Shujie Li, Hao Hong

Zhi-Qiang Ding et al 2026 The Astrophysical Journal Letters 1012 .

  • Provider: AAS Journals

Caption: Figure F7.

Spectral identification of an emission line feature (Tref + 237–246 s). The analysis incorporates unsaturated observations from HEPP-H, GECAM-C, and Fermi/GBM. (a) The count spectrum. (b) The νFν spectral distribution (units of keV2 · photons · cm−2 · s−1 · keV−1). (c) Residuals in units of standard deviation (σ) with 1σ error bars. Solid lines indicate the best-fitting model (Band function + Gaussian line), while dashed lines denote individual components. Time intervals indicated in parentheses are relative to Tref.

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