HXMT Identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428

• Published in: arXiv.org 2021-04
• Main Authors: Lin, L, Xiong, S L, Ge, M Y, Li, X B, Li, T P, Lu, F J, Zhang, S N, Tuo, Y L, Nang, Y, Xiao, S, Chen, Y, Song, L M, Jia, S M, Cao, X L, Qu, J L, Zhang, S, Gu, Y D, Liao, J Y, Zhao, X F, Tan, Y, Nie, J Y, Zhao, H S, Zheng, S J, Luo, Q, B Li, Xue, W C, Bu, Q C, Chen, G, Chen, T X, Chen, Y B, Chen, Y P, Cui, W, Cui, W W, Deng, J K, Dong, Y W, Du, Y Y, Fu, M X, Gao, G H, Gao, H, Gao, M, Guan, J, Guo, C C, Han, D W, Jiang, L H, Jin, J, Jin, Y J, Kong, L D, G Li, Li, M S, W Li, X Li, Li, X F, Li, Y G, Li, Z W, Liu, B S, Liu, G Q, Liu, H W, Liu, X J, Liu, Y N, B Lu, Lu, X F, Luo, T, X Ma, Meng, B, G Ou, Sai, N, Shang, R C, Song, X Y, Sun, L, Tao, L, Wang, J, Wang, W S, Wang, Y S, Wen, X Y, Wu, B B, Wu, B Y, M Wu, H Xu, Yang, S, Yang, Y J, Yi, Q B, You, Y, Zhang, A M, Zhang, C M, Zhang, F, Zhang, H M, Zhang, J, Zhang, T, Zhang, W, Zhang, W C, Zhang, W Z, Zhang, Y F, Zhang, Y J, Zhang, Z, Zhang, Zhi, Zhang, Z L, Zhou, D K, Zhou, J F, Zhu, Y X, Zhuang, R L
• Format: Article
• Language: English
• Subjects: Delay time; Energy bands; Gamma rays; High energy astronomy; Magnetars; Neutron stars; Radio bursts; Repeaters; Separation; Short pulses; Stellar magnetic fields; Stellar rotation
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2005.11071

Fast radio bursts (FRBs) are short pulses observed in radio band from cosmological distances. One class of models invoke soft gamma-ray repeaters (SGRs), or magnetars, as the sources of FRBs. Some radio pulses have been observed from some magnetars, however, no FRB-like events had been detected in association any magnetar burst, including one giant flare. Recently, a pair of FRB-like bursts (FRB 200428 hereafter) separated by milliseconds (ms) were detected from the general direction of the Galactic magnetar SGR J1935+2154. Here we report the detection of a non-thermal X-ray burst in the 1-250 keV energy band with the Insight-HXMT satellite, which we identify as emitted from SGR J1935+2154. The burst showed two hard peaks with a separation of 34 ms, broadly consistent with that of the two bursts in FRB 200428. The delay time between the double radio and X-ray peaks is about 8.57 s, fully consistent with the dispersion delay of FRB 200428. We thus identify the non-thermal X-ray burst is associated with FRB 200428 whose high energy counterpart is the two hard peaks in X-ray. Our results suggest that the non-thermal X-ray burst and FRB 200428 share the same physical origin in an explosive event from SGR J1935+2154.