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    Constraints on the cosmic-ray electron spectrum above 25 TeV from the LHAASO experiment

    Zhen Cao1,2,3, F. Aharonian4,5, Axikegu6, Y. X. Bai1,3, Y. W. Bao7, D. Bastieri8, X. J. Bi1,2,3, Y. J. Bi1,3, W. Bian9 et al. (LHAASO Collaboration)

    W. Bian9, A. V. Bukevich10, Q. Cao11, W. Y. Cao12, Zhe Cao13,12, J. Chang14, J. F. Chang1,3,13, A. M. Chen9, E. S. Chen1,2,3, H. X. Chen15, Liang Chen16, Lin Chen6, Long Chen6, M. J. Chen1,3, M. L. Chen1,3,13, Q. H. Chen6, S. Chen17, S. H. Chen1,2,3, S. Z. Chen1,3, T. L. Chen18, Y. Chen7, N. Cheng1,3, Y. D. Cheng1,2,3, M. C. Chu19, M. Y. Cui14, S. W. Cui11, X. H. Cui20, Y. D. Cui21, B. Z. Dai17, H. L. Dai1,3,13, Z. G. Dai12, Danzengluobu18, X. Q. Dong1,2,3, K. K. Duan14, J. H. Fan8, Y. Z. Fan14, J. Fang17, J. H. Fang15, K. Fang1,3, C. F. Feng22, H. Feng1, L. Feng14, S. H. Feng1,3, X. T. Feng22, Y. Feng15, Y. L. Feng18, S. Gabici23, B. Gao1,3, C. D. Gao22, Q. Gao18, W. Gao1,3, W. K. Gao1,2,3, M. M. Ge17, T. T. Ge21, L. S. Geng1,3, G. Giacinti9, G. H. Gong24, Q. B. Gou1,3, M. H. Gu1,3,13, F. L. Guo16, J. Guo24, X. L. Guo6, Y. Q. Guo1,3, Y. Y. Guo14, Y. A. Han25, O. A. Hannuksela19, M. Hasan1,2,3, H. H. He1,2,3,*, H. N. He14, J. Y. He14, Y. He6, Y. K. Hor21, B. W. Hou1,2,3, C. Hou1,3, X. Hou26, H. B. Hu1,2,3, Q. Hu12,14, S. C. Hu1,3,27, C. Huang7, D. H. Huang6, T. Q. Huang1,3, W. J. Huang21, X. T. Huang22, X. Y. Huang14, Y. Huang1,2,3, Y. Y. Huang7, X. L. Ji1,3,13, H. Y. Jia6, K. Jia22, H. B. Jiang1,3, K. Jiang13,12, X. W. Jiang1,3, Z. J. Jiang17, M. Jin6, M. M. Kang28, I. Karpikov10, D. Khangulyan1,3, D. Kuleshov10, K. Kurinov10, B. B. Li11, C. M. Li7, Cheng Li13,12, Cong Li1,3, D. Li1,2,3, F. Li1,3,13, H. B. Li1,3, H. C. Li1,3, Jian Li12, Jie Li1,3,13, K. Li1,3, S. D. Li16,2, W. L. Li22, W. L. Li9, X. R. Li1,3, Xin Li13,12, Y. Z. Li1,2,3, Zhe Li1,3, Zhuo Li29, E. W. Liang30, Y. F. Liang30, S. J. Lin21, B. Liu12, C. Liu1,3, D. Liu22, D. B. Liu9, H. Liu6, H. D. Liu25, J. Liu1,3, J. L. Liu1,3, M. Y. Liu18, R. Y. Liu7, S. M. Liu6, W. Liu1,3, Y. Liu8, Y. N. Liu24, Q. Luo21, Y. Luo9, H. K. Lv1,3, B. Q. Ma29, L. L. Ma1,3, X. H. Ma1,3, J. R. Mao26, Z. Min1,3, W. Mitthumsiri31, H. J. Mu25, Y. C. Nan1,3, A. Neronov23, K. C. Y. Ng19, L. J. Ou8, P. Pattarakijwanich31, Z. Y. Pei8, J. C. Qi1,2,3, M. Y. Qi1,3, B. Q. Qiao1,3, J. J. Qin12, A. Raza1,2,3, D. Ruffolo31, A. Sáiz31, M. Saeed1,2,3, D. Semikoz23, L. Shao11, O. Shchegolev10,32, X. D. Sheng1,3, F. W. Shu33, H. C. Song29, Yu. V. Stenkin10,32, V. Stepanov10, Y. Su14, D. X. Sun12,14, Q. N. Sun6, X. N. Sun30, Z. B. Sun34, J. Takata35, P. H. T. Tam21, Q. W. Tang33, R. Tang9, Z. B. Tang13,12, W. W. Tian2,20, L. H. Wan21, C. Wang34, C. B. Wang6, G. W. Wang12, H. G. Wang8, H. H. Wang21, J. C. Wang26, Kai Wang7, Kai Wang35, L. P. Wang1,2,3, L. Y. Wang1,3, P. H. Wang6, R. Wang22, W. Wang21, X. G. Wang30, X. Y. Wang7, Y. Wang6, Y. D. Wang1,3, Y. J. Wang1,3, Z. H. Wang28, Z. X. Wang17, Zhen Wang9, Zheng Wang1,3,13, D. M. Wei14, J. J. Wei14, Y. J. Wei1,2,3, T. Wen17, C. Y. Wu1,3, H. R. Wu1,3, Q. W. Wu35, S. Wu1,3,†, X. F. Wu14, Y. S. Wu12, S. Q. Xi1,3, J. Xia12,14, G. M. Xiang16,2, D. X. Xiao11, G. Xiao1,3, Y. L. Xin6, Y. Xing16, D. R. Xiong26, Z. Xiong1,2,3,‡, D. L. Xu9, R. F. Xu1,2,3, R. X. Xu29, W. L. Xu28, L. Xue22, D. H. Yan17, J. Z. Yan14, T. Yan1,3, C. W. Yang28, C. Y. Yang26, F. Yang11, F. F. Yang1,3,13, L. L. Yang21, M. J. Yang1,3, R. Z. Yang12, W. X. Yang8, Y. H. Yao1,3, Z. G. Yao1,3, L. Q. Yin1,3, N. Yin22, X. H. You1,3, Z. Y. You1,3, Y. H. Yu12, Q. Yuan14, H. Yue1,2,3, H. D. Zeng14, T. X. Zeng1,3,13, W. Zeng17, M. Zha1,3, B. B. Zhang7, F. Zhang6, H. Zhang9, H. M. Zhang7, H. Y. Zhang17, J. L. Zhang20, Li Zhang17, P. F. Zhang17, P. P. Zhang12,14, R. Zhang14, S. B. Zhang2,20, S. R. Zhang11, S. S. Zhang1,3, X. Zhang7, X. P. Zhang1,3, Y. F. Zhang6, Yi Zhang1,14, Yong Zhang1,3, B. Zhao6, J. Zhao1,3, L. Zhao13,12, L. Z. Zhao11, S. P. Zhao14, X. H. Zhao26, F. Zheng34, W. J. Zhong7, B. Zhou1,3, H. Zhou9, J. N. Zhou16, M. Zhou33, P. Zhou7, R. Zhou28, X. X. Zhou1,2,3, X. X. Zhou6, B. Y. Zhu12,14, C. G. Zhu22, F. R. Zhu6, H. Zhu20, K. J. Zhu1,2,3,13, Y. C. Zou35, and X. Zuo1,3 (LHAASO Collaboration)

    • 1Key Laboratory of Particle Astrophysics and Experimental Physics Division and Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, 100049 Beijing, China
    • 2University of Chinese Academy of Sciences, 100049 Beijing, China
    • 3TIANFU Cosmic Ray Research Center, Chengdu, Sichuan, China
    • 4Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, 2 Dublin, Ireland
    • 5Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, 69029 Heidelberg, Germany
    • 6School of Physical Science and Technology and School of Information Science and Technology, Southwest Jiaotong University, 610031 Chengdu, Sichuan, China
    • 7School of Astronomy and Space Science, Nanjing University, 210023 Nanjing, Jiangsu, China
    • 8Center for Astrophysics, Guangzhou University, 510006 Guangzhou, Guangdong, China
    • 9Tsung-Dao Lee Institute and School of Physics and Astronomy, Shanghai Jiao Tong University, 200240 Shanghai, China
    • 10Institute for Nuclear Research of Russian Academy of Sciences, 117312 Moscow, Russia
    • 11Hebei Normal University, 050024 Shijiazhuang, Hebei, China
    • 12University of Science and Technology of China, 230026 Hefei, Anhui, China
    • 13State Key Laboratory of Particle Detection and Electronics, Beijing, China
    • 14Key Laboratory of Dark Matter and Space Astronomy and Key Laboratory of Radio Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210023 Nanjing, Jiangsu, China
    • 15Research Center for Astronomical Computing, Zhejiang Laboratory, 311121 Hangzhou, Zhejiang, China
    • 16Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 200030 Shanghai, China
    • 17School of Physics and Astronomy, Yunnan University, 650091 Kunming, Yunnan, China
    • 18Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education, 850000 Lhasa, Tibet, China
    • 19Department of Physics, The Chinese University of Hong Kong, Shatin, New Territories, Hong Kong, China
    • 20Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China
    • 21School of Physics and Astronomy (Zhuhai) and School of Physics (Guangzhou) and Sino-French Institute of Nuclear Engineering and Technology (Zhuhai), Sun Yat-sen University, 519000 Zhuhai, 510275 Guangzhou, Guangdong, China
    • 22Institute of Frontier and Interdisciplinary Science, Shandong University, 266237 Qingdao, Shandong, China
    • 23APC, Université Paris Cité, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, 119 75205 Paris, France
    • 24Department of Engineering Physics and Department of Astronomy, Tsinghua University, 100084 Beijing, China
    • 25School of Physics and Microelectronics, Zhengzhou University, 450001 Zhengzhou, Henan, China
    • 26Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, Yunnan, China
    • 27China Center of Advanced Science and Technology, Beijing 100190, China
    • 28College of Physics, Sichuan University, 610065 Chengdu, Sichuan, China
    • 29School of Physics, Peking University, 100871 Beijing, China
    • 30Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, 530004 Nanning, Guangxi, China
    • 31Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400, Thailand
    • 32Moscow Institute of Physics and Technology, 141700 Moscow, Russia
    • 33Center for Relativistic Astrophysics and High Energy Physics, School of Physics and Materials Science and Institute of Space Science and Technology, Nanchang University, 330031 Nanchang, Jiangxi, China
    • 34National Space Science Center, Chinese Academy of Sciences, 100190 Beijing, China
    • 35School of Physics, Huazhong University of Science and Technology, Wuhan 430074, Hubei, China

    • *Contact author: hhh@ihep.ac.cn
    • †Contact author: wusha@ihep.ac.cn
    • ‡Contact author: xiongzheng@ihep.ac.cn
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    Phys. Rev. D 112, 022007 – Published 31 July, 2025

    DOI: https://doi.org/10.1103/wy2f-b9p3

    Abstract

    Cosmic-ray electrons and positrons (CREs) offer valuable insights into the origins of local cosmic rays, as they rapidly cool in interstellar magnetic and radiation fields, limiting their propagation range. The CRE spectrum reveals a spectral break around 1 TeV, followed by a continuous power-law behavior that possibly extends beyond 40 TeV. Deviations from a pure power-law in this spectrum could provide important clues about the local origins of CREs. However, due to the rapidly falling flux of CRE, the ratio of hadron/CRE increases with energy, making the rejection more and more challenging. Equipped with a large detection aperture and strong background rejection capability, LHAASO has the potential to extend CRE spectrum measurements beyond 25 TeV, which is almost the highest energy measured by existing experiments. In this work, we study the detector performance and explore the optimized background rejection of cosmic nuclei background specifically for CRE observations in LHAASO. Our analysis reveals that muon-poor nuclei showers have a strong dependence on the hadronic model when estimating the cosmic nuclei background and rejection capability. Consequently, we derived a 90% CL upper limit for the CRE spectrum from 25 to 160 TeV, providing a new and restrictive constraint in the hundreds of TeV range for the first time.

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    Phys. Rev. D 112, 022007– Published 31 July, 2025
    • Received 12 December 2024
    • Accepted 23 June 2025
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