Reconstruction of Cherenkov image by multiple telescopes of LHAASO-WFCTA

F. Aharonian, Q. An, Axikegu, L. X. Bai, Y. X. Bai, Y. W. Bao,D. Bastieri,X. J. Bi,Y. J. Bi, J. T. Cai,Zhe Cao,Zhen Cao,J. Chang,J. F. Chang,E. S. Chen,Liang Chen,Liang Chen,Long Chen,M. J. Chen,M. L. Chen,Q. H. Chen,S. H. Chen,S. Z. Chen,T. L. Chen,Y. Chen,H. L. Cheng, 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,K. K. Duan,J. H. Fan,Y. Z. Fan,Z. X. Fan, J. Fang, K. Fang, C. F. Feng,L. Feng,S. H. Feng, X. T. Feng,Y. L. Feng, B. Gao, C. D. Gao, L. Q. Gao, Q. Gao, W. Gao, W. K. 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, S. L. He,X. B. He, Y. He, M. Heller,Y. K. Hor, C. Hou, X. Hou, H. B. Hu,Q. Hu,S. Hu,S. C. Hu,X. J. Hu,D. H. Huang,W. H. Huang,X. T. Huang,X. Y. Huang,Y. Huang,Z. C. Huang,X. L. Ji, H. Y. Jia, K. Jia, K. Jiang, Z. J. Jiang,M. Jin, M. M. Kang,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,Jian Li,Jie Li,K. Li,W. L. Li,X. R. Li,Xin 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. S. Liu,J. Y. Liu,M. Y. Liu,R. Y. Liu,S. M. Liu,W. Liu, Y. Liu,Y. N. Liu, W. J. Long, R. Lu, Q. Luo,H. K. Lv, B. Q. Ma,L. L. Ma, X. H. Ma, J. R. Mao, A. Masood, Z. Min,W. Mitthumsiri, Y. C. Nan, 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. Sáiz, C. Y. Shao, L. Shao, O. Shchegolev, X. D. Sheng, J. Y. Shi, H. C. Song,Yu. V. 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. Wang,R. N. Wang,W. Wang,X. G. 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,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. X. Xu, L. Xue,D. H. Yan,J. Z. Yan, C. W. 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, Z. K. Zeng,M. Zha, X. X. Zhai, B. B. Zhang,F. Zhang,H. M. Zhang,H. Y. Zhang,J. L. Zhang,L. X. Zhang,Li Zhang,Lu 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,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

RADIATION DETECTION TECHNOLOGY AND METHODS（2022）

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摘要

Introduction One of main scientific goals of the Large High Altitude Air Shower Observatory (LHAASO) is to accurately measure the energy spectra of different cosmic ray compositions around the ‘knee’ region. The Wide Field-of-View (FoV) Cherenkov Telescope Array (WFCTA), which is one of the main detectors of LHAASO and has 18 telescopes, is built to achieve this goal. Multiple telescopes are put together and point to connected directions for a larger FoV. Method Telescopes are deployed spatially as close as possible, but due to their own size, the distance between two adjacent telescopes is about 10 m. Therefore, the Cherenkov lateral distribution and the parallax between the two telescopes should be considered in the event building process for images crossing over the boundaries of FoVs of the telescopes. An event building method for Cherenkov images measured by multiple telescopes of WFCTA is developed. The performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in simulation. Results and conclusion It is proved that the developed event building process can help to increase the FoV of WFCTA by 30% while maintaining the same reconstruction quality, compared to the separate telescope reconstruction method.

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cherenkov image,multiple telescopes,lhaaso-wfcta

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