An Ultrahigh-Energy Γ-Ray Bubble Powered by a Super PeVatron

Z. Cao,F. Aharonian,Q. An, Axikegu,Y. X. Bai,Y. W. Bao,D. Bastieri,X. J. Bi, Y. J. Bi,J. T. Cai,Q. Cao,W. Y. Cao,Zhe Cao,J. Chang,J. F. Chang, A. M. Chen,E. S. Chen,Liang Chen,Lin Chen,Long Chen, M. J. Chen,M. L. Chen,Q. H. Chen,S. H. Chen,S. Z. Chen,T. L. Chen,Y. Chen,N. Cheng,Y. D. Cheng,M. Y. Cui,S. W. Cui,X. H. Cui,Y. D. Cui,B. Z. Dai,H. L. Dai,Z. G. Dai, Danzengluobu,D. della Volpe,X. Q. Dong,K. K. Duan,J. H. Fan,Y. Z. Fan,J. Fang,K. Fang,C. F. Feng,L. Feng,S. H. Feng,X. T. Feng,Y. L. Feng, S. Gabici,B. Gao,C. D. Gao,L. Q. Gao,Q. Gao,W. Gao,W. K. Gao,M. M. Ge,L. S. Geng,G. Giacinti,G. H. Gong,Q. B. Gou, M. H. Gu,F. L. Guo,X. L. Guo,Y. Q. Guo,Y. Y. Guo,Y. A. Han,H. H. He,H. N. He,J. Y. He,X. B. He,Y. He,M. Heller,Y. K. Hor,B. W. Hou,C. Hou,X. Hou,H. B. Hu, Q. Hu,S. C. Hu, D. H. Huang, T. Q. Huang,W. J. Huang, X. T. Huang,X. Y. Huang,Y. Huang,Z. C. Huang,X. L. Ji,H. Y. Jia,K. Jia,K. Jiang,X. W. Jiang,Z. J. Jiang,M. Jin,M. M. Kang,T. Ke,D. Kuleshov,K. Kurinov,B. B. Li,Cheng Li,Cong Li,D. Li,F. Li,H. B. Li,H. C. Li, H. Y. Li,J. Li,Jian Li,Jie Li, K. Li,W. L. Li,X. R. Li,Xin Li,Y. Z. Li,Zhe Li,Zhuo Li,E. W. Liang,Y. F. Liang,S. J. Lin,B. Liu, C. Liu, D. Liu,H. Liu,H. D. Liu, J. Liu, J. L. Liu,J. Y. Liu,M. Y. Liu,R. Y. Liu,S. M. Liu,W. Liu,Y. Liu,Y. N. Liu,R. Lu,Q. Luo,H. K. Lv,B. Q. Ma,L. L. Ma,X. H. Ma,J. R. Mao,Z. Min,W. Mitthumsiri,H. J. Mu,Y. C. Nan,A. Neronov,Z. W. Ou,B. Y. Pang,P. Pattarakijwanich, Z. Y. Pei,M. Y. Qi,Y. Q. Qi,B. Q. Qiao,J. J. Qin,D. Ruffolo,A. Saiz,D. Semikoz,C. Y. Shao,L. Shao,O. Shchegolev,X. D. Sheng,F. W. Shu,H. C. Song,Yu. V. Stenkin,V. Stepanov,Y. Su,Q. N. Sun,X. N. Sun,Z. B. Sun, P. H. T. Tam,Q. W. Tang,Z. B. Tang,W. W. Tian,C. Wang,C. B. Wang,G. W. Wang, H. G. Wang, H. H. Wang,J. C. Wang,K. Wang, L. P. Wang, L. Y. Wang, P. H. Wang, R. Wang,W. Wang, X. G. Wang, X. Y. Wang,Y. Wang,Y. D. Wang, Y. J. Wang,Z. H. Wang,Z. X. Wang,Zhen Wang,Zheng Wang,D. M. Wei,J. J. Wei,Y. J. Wei,T. Wen,C. Y. Wu,H. R. Wu,S. Wu,X. F. Wu,Y. S. Wu,S. Q. Xi,J. Xia,J. J. Xia,G. M. Xiang,D. X. Xiao,G. Xiao,G. G. Xin,Y. L. Xin,Y. Xing,Z. Xiong,D. L. Xu,R. F. Xu,R. X. Xu,W. L. Xu,L. Xue,D. H. Yan,J. Z. Yan,T. Yan,C. W. Yang,F. Yang,F. F. Yang,H. W. Yang,J. Y. Yang,L. L. Yang, M. J. Yang,R. Z. Yang,S. B. Yang,Y. H. Yao,Z. G. Yao,Y. M. Ye,L. Q. Yin,N. Yin, X. H. You,Z. Y. You,Y. H. Yu,Q. Yuan,H. Yue,H. D. Zeng,T. X. Zeng,W. Zeng,M. Zha,B. B. Zhang,F. Zhang, H. M. Zhang,H. Y. Zhang,J. L. Zhang, L. X. Zhang,Li Zhang, P. F. Zhang,P. P. Zhang,R. Zhang,S. B. Zhang,S. R. Zhang,S. S. Zhang,X. Zhang,X. P. Zhang,Y. F. Zhang,Yi Zhang,Yong Zhang,B. Zhao,J. Zhao,L. Zhao,L. Z. Zhao,S. P. Zhao,F. Zheng, B. Zhou,H. Zhou,J. N. Zhou,M. Zhou,P. Zhou,R. Zhou,X. X. Zhou,C. G. Zhu,F. R. Zhu,H. Zhu,K. J. Zhu,X. Zuo

SCIENCE BULLETIN（2024）

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摘要

We report the detection of a y-ray bubble spanning at least 100 deg2 in ultra-high energy (UHE) up to a few PeV in the direction of the star-forming region Cygnus X, implying the presence super PeVatron(s) accelerating protons to at least 10 PeV. A log-parabola form with the photon index C(E) = (2.71 +/- 0.02) + (0.11 +/- 0.02) x log10(E/10 TeV) is found fitting the gamma-ray energy spectrum of the bubble well. UHE sources, "hot spots" correlated with very massive molecular clouds, and a quasi-spherical amorphous y-ray emitter with a sharp central brightening are observed in the bubble. In the core of - 0.5 degrees, spatially associating with a region containing massive OB association (Cygnus OB2) and a microquasar (Cygnus X-3), as well as previously reported multi-TeV sources, an enhanced concentration of UHE y-rays is observed with 2 photons at energies above 1 PeV. The general feature of the bubble, the morphology, and the energy spectrum, are reasonably reproduced by the assumption of a particle accelerator in the core, continuously injecting protons into the ambient medium. (c) 2023 Science China Press. Published by Elsevier B.V. and Science China Press. All rights reserved.

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Cosmic rays,y-rays,Interstellar medium,Star cluster

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