Discovery Of A New Gamma-Ray Source, Lhaaso J0341+5258, With Emission Up To 200 Tev

Zhen Cao,F. Aharonian, Q. An, Axikegu,L. X. Bai, Y. X. Bai, Y. W. Bao,D. Bastieri,X. J. Bi,Y. J. Bi, H. Cai, J. T. Cai,Zhe Cao,J. Chang,J. F. Chang,B. M. Chen,E. S. Chen,J. Chen,Liang Chen, Long Chen,M. J. Chen,M. L. Chen,Q. H. Chen, S. H. Chen,S. Z. Chen,T. L. Chen,X. L. Chen,Y. Chen, N. Cheng,Y. D. Cheng, S. W. Cui,X. H. Cui,Y. D. Cui,B. D'Ettorre Piazzoli,B. Z. Dai,H. L. Dai,Z. G. Dai, Danzengluobu,D. Della Volpe,X. J. Dong,K. K. Duan,J. H. Fan,Y. Z. Fan,Z. X. Fan, J. Fang, K. Fang, C. F. Feng,L. Feng,S. H. Feng,Y. L. Feng, B. Gao, C. D. Gao, L. Q. Gao, Q. Gao, W. Gao, M. M. Ge, L. S. Geng,G. H. Gong, Q. B. Gou, M. H. Gu,F. L. Guo,J. G. Guo,X. L. Guo,Y. Q. Guo,Y. Y. Guo,Y. A. Han,H. H. He,H. N. He, J. C. He,S. L. He,X. B. He,Y. He,M. Heller,Y. K. Hor,C. Hou,H. B. Hu,S. Hu,S. C. Hu, X. J. Hu,D. H. Huang,Q. L. Huang,W. H. Huang,X. T. Huang,X. Y. Huang,Z. C. Huang,F. Ji,X. L. Ji,H. Y. Jia,K. Jiang,Z. J. Jiang, C. Jin,T. Ke,D. Kuleshov, K. Levochkin,B. B. Li, Cheng Li,Cong Li,F. Li,H. B. Li,H. C. Li,H. Y. Li, J. Li, K. Li,W. L. Li,X. R. Li,Xin Li,Y. 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. S. Liu,J. Y. Liu,M. Y. Liu, R. Y. Liu,S. M. Liu, W. Liu, Y. Liu, Y. N. Liu, Z. X. Liu, W. J. Long,R. Lu,H. K. Lv, B. Q. Ma,L. L. Ma, X. H. Ma, J. R. Mao,A. Masood, Z. Min,W. Mitthumsiri,T. Montaruli, Y. C. Nan, B. Y. Pang, P. Pattarakijwanich,Z. Y. Pei,M. Y. Qi,Y. Q. Qi, B. Q. Qiao, J. J. Qin,D. Ruffolo, V Rulev,A. Saiz,L. Shao, O. Shchegolev, X. D. Sheng,J. Y. Shi, H. C. Song,Yu Stenkin,V Stepanov,Y. Su,Q. N. Sun,X. N. Sun,Z. B. Sun,P. H. T. Tam,Z. B. Tang,W. W. Tian,B. D. Wang,C. Wang, H. Wang, H. G. Wang,J. C. Wang, J. S. Wang,L. P. Wang,L. Y. Wang, R. N. Wang, W. Wang, X. G. Wang, X. J. Wang, X. Y. Wang, Y. Wang, Y. D. Wang, Y. J. Wang, Y. P. 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, W. X. Wu,X. F. Wu, S. Q. Xi,J. Xia,J. J. Xia, G. M. Xiang, D. X. Xiao, G. Xiao, H. B. Xiao, G. G. Xin,Y. L. Xin,Y. Xing,D. L. Xu,R. X. Xu, L. Xue,D. H. Yan,J. Z. Yan, C. W. Yang, F. F. 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. D. Zeng,T. X. Zeng,W. Zeng, Z. K. Zeng,M. Zha, X. X. Zhai,B. B. Zhang,H. M. Zhang,H. Y. Zhang,J. L. Zhang,J. W. Zhang,L. X. Zhang,Li Zhang, Lu Zhang,P. F. Zhang,P. P. Zhang,R. Zhang,S. R. Zhang,S. S. Zhang, X. Zhang, X. P. Zhang,Y. F. Zhang,Y. L. Zhang,Yi Zhang,Yong Zhang,B. Zhao,J. Zhao, L. Zhao, L. Z. Zhao,S. P. Zhao,F. Zheng, Y. Zheng, B. Zhou,H. Zhou,J. N. Zhou,P. Zhou,R. Zhou, X. X. Zhou, C. G. Zhu, F. R. Zhu,H. Zhu, K. J. Zhu,X. Zuo

arxiv（2021）

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摘要

We report the discovery of a new unidentified extended gamma-ray source in the Galactic plane named LHAASO J0341+5258 with a pretrial significance of 8.2 standard deviations above 25 TeV. The best-fit position is R.A. = 55.degrees 34 +/- 0.degrees 11 and decl. = 52.degrees 97 +/- 0.degrees 07. The angular size of LHAASO J0341+5258 is 0.degrees 29 +/- 0.degrees 06(stat) +/- 0.degrees 02(sys). The flux above 25 TeV is about 20% of the flux of the Crab Nebula. Although a power-law fit of the spectrum from 10 to 200 TeV with the photon index alpha = 2.98 +/- 0.19(stat) +/- 0.02(sys) is not excluded, the LHAASO data together with the flux upper limit at 10 GeV set by the Fermi-LAT observation, indicate a noticeable steepening of an initially hard power-law spectrum with a cutoff at approximate to 50 TeV. We briefly discuss the origin of ultra-high-energy gamma rays. The lack of an energetic pulsar and a young supernova remnant inside or in the vicinity of LHAASO J0341+5258 challenge, but do not exclude, both the leptonic and hadronic scenarios of gamma-ray production.

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lhaaso j0341+5258,emission,gamma-ray

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