Accès ouvert déclaré
2025
preprint
A Giant Peanut-shaped Ultra-High-Energy Gamma-Ray Emitter Off the Galactic Plane
Zhen Cao, F. Aharonian, Y.X Bai, Y. W. Bao, D. Bastieri, Xiao-Jun Bi, Y. J. Bi, Wenyu Cao, Zhe Cao, M. Chen, Ensheng Chen, G.H Chen, H. X. Chen, Liang Chen, Long Chen, Mingjun Chen, Min Chen, Qi-Hui Chen, S. Z. Chen, Tianlu Chen, Yang Chen, Ning Cheng, M. C. Chu, Maxwell Cui, S. W. Cui, Xiaohong Cui, B. Z. Dai, H. L. Dai, Z. G. Dai, Danzengluobu, X. Q. Dong, Junhui Fan, Yi-Zhong Fan, Jun Fang, Jian-Hua Fang, Kun Fang, Hua Feng, Lei Feng, Shaohui Feng, X.T Feng, Yi Feng, Y. L. Feng, S. Gabici, Bo Gao, Qi Gao, Wei Gao, W. K. Gao, M. M. Ge, Ting-Ting Ge, Lisi Geng, Gwenael Giacinti, Guanghua Gong, Q. B. Gou, Minhao Gu, Jing Guo, Y. Y. Guo, O. A. Hannuksela, M Hasan, H. H. He, Hao-Ning He, Jiayu He, Xu He, Y. He, Sergio Hernández Cadena, Chuan Hou, Hongbo Hu, S. Hu, Chen Huang, Daihui Huang, Jiajun Huang, Tian-Qi Huang, Wenjun Huang, Xingtao Huang, X.Y Huang, Yi-Yun Huang, X. L. Ji, H. Y. Jia, Jia Kang, H. B. Jiang, K. Jiang, Xiaowei Jiang, Z. J. Jiang, Min Jin, S Kaci, Ming-Ming Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, Bingbing Li, Cheng Li, Cong Li, Di Li, Fei Li, Haibo Li, Huicai Li, J. Li, Jie Li, Ke Li, Long Li, R.L Li, S. D. Li, T.Y Li, Weimin Li, Xiurong Li, Xin Li, Yizhuo Li, Yuan Li, Zhe Li, Zhuo Li, En-Wei Liang, Yunfeng Liang, Sujie Lin, Bing Liu, Cheng Liu, Dong Liu, D. Liu, H. Liu, Haidong Liu, Jia Liu, J.L Liu, Ruoyu Liu, Siming Liu, Wei Liu, Xi Liu, M.Y. Liu, Yu Liu, Yinong Liu, Yangping Luo, H. K. Lv, Bo-Qiang Ma, L.L. Ma, X. H., J. Mao, Ziying Min, W. Mitthumsiri, Guobin Mou, H. J. Mu, A. Neronov, Kenny C. Y. Ng, Mingyang Ni, Miaoling Ou, P. Pattarakijwanich, Jiesong Qi, M. Y. Qi, Jiajun Qin, Ali Raza, Chongyang Ren, D. Ruffolo, A. Sáiz, D. Semikoz, O. Shchegolev, Yunzhi Shen, X. D. Sheng, Zhaodong Shi, F.W. 富文 Shu 舒, Huichao Song, Xiaona Sun, P. H. T. Tam, Qingwen Tang, Ruiyi Tang, Chao Wang, Guangwei Wang, H. G. Wang, Jiancheng Wang, Ke Wang, K Wang, Kai Wang, Liping Wang, Luyao Wang, Ran Wang, Wei Wang, Xinjian Wang, Xiang‐Yu Wang, Yudong Wang, Y.D Wang, Zhongxiang Wang, Zheng Wang, Shanshan Weng, C. Y. Wu, Qingwen Wu, Qinmu Wu, Xue-Feng Wu, Y. Wu, J. Xia, Junji Xia, Di-Xuan Xiao, Gang Xiao, Y. L. Xin, Dingrong Xiong, Renfeng Xu, R.F Xu, Weili Xu, T. Yan, Fengfan Yang, Ruizhi Yang, Meimei Yang, Z. Yang, X. H. Ye, Na Yin, Hua Yue, Houdun Zeng, Tingxuan Zeng, Xiangtao Zeng, M. Zha, Binbin Zhang, Chao Zhang, Hongfei Zhang, Haiming Zhang, Hengying Zhang, Jianli Zhang, Li Zhang, Li Zhang, P.P Zhang, Shoushan Zhang, Weiyan Zhang, W.Y Zhang, Yi Zhang, Zhipeng Zhang, Lei Zhao, Lizhi Zhao, Xiaohong Zhao, H. Zhou, Meng Zhou, Ping Zhou, P. Zhou, Grace Zhou, Xunxiu ZHOU, Ben-Yang Zhu, Chengguang Zhu, Fengrong Zhu, Kejun Zhu, Oscar Macías
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Résumé fourni par la source
Ultra-high-energy (UHE), exceeding 100 TeV (10^12 electronvolts), γ-rays manifests extreme particle acceleration in astrophysical sources. Recent observations by γ-ray telescopes, particularly by the Large High Altitude Air Shower Observatory (LHAASO), have revealed a few tens of UHE sources, indicating numerous Galactic sources capable of accelerating particles to PeV (10^15 electronvolts) energies. However, discerning the dominant acceleration mechanisms (leptonic versus hadronic), the relative contributions of specific source classes, and the role of particle transport in shaping their observed emission are central goals of modern UHE astrophysics. Here we report the discovery of a giant UHE γ-ray emitter at -17.5° off the Galactic plane - a region where UHE γ-ray sources are rarely found. The emitter exhibits a distinctive asymmetric shape, resembling a giant "Peanut" spanning 0.45° \times 4.6°, indicative of anisotropic particle distribution over a large area. A highly aged millisecond pulsar (MSP) J0218+4232 is the sole candidate accelerator positionally coincident with the Peanut region. Its association with UHE γ-rays extending to 0.7 PeV, if confirmed, would provide the first evidence of a millisecond pulsar powering PeV particles. Such a finding challenges prevailing models, which posit that millisecond pulsars cannot sustain acceleration to PeV energies. The detection reveals fundamental gaps in understanding particle acceleration, cosmic-ray transport, and interstellar magnetic field effects, potentially revealing new PeV accelerator (PeVatron) classes.
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Sujets associés
Astrophysics and Cosmic PhenomenaRadiation Effects and DosimetryGamma-ray bursts and supernovae