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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 2.

Joint spectral characterization of GRB 221009A across multiple time periods. (a)–(c) Analysis for the high-flux peak phase (Tref + 228–230 s) utilizing a Band + BB model. (d)–(f) Spectral analysis for the late decay phase (Tref + 246–256 s) utilizing a multicomponent Band + Gaussian model. Panels (a) and (d) show observed count rate spectra compared with the folded best-fit models (solid lines). Data are from GECAM-C (high-gain in green; low-gain in orange), Fermi/GBM bismuth germanate (BGO) detectors (b0 in purple; b1 in blue) and HEPP-H (gray). Panels (b) and (e) show the νFν spectral distribution (units of keV2 · photons · cm−2 · s−1 · keV−1). For the peak phase (b), the displayed spectrum is fitted with the Band + BB model. For the late phase (e), the model includes a Band tail and a Gaussian line feature centered near 37 MeV. In both time periods, HEPP-H data (gray) span the 2–255 MeV energy range. Panels (c) and (f) show residuals in units of standard deviation (σ) with 1σ error bars.

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