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

Aharonian, F.; An, Q.; Axikegu,; Bai, Lixin; Bai, Y.; Bao, Yiwei; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao, Z.; Cao, Zhe; Chang, Jin; Chen, 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.; Cheng, Ning; Cheng, Yaodong; Cui, S. W.; Cui, Xiaohong; Cui, Yudong; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu,; Volpe, D. della; Piazzoli, B. D’Ettorre; Dong, X.; Duan, Kai-Kai; Fan, J. H.; Fan, Yi‐Zhong; Zhou, Fan; Fang, J.; Fang, Ke; Feng, C. F.; Feng, Li; Feng, S. H.; Feng, Y. L.; Gao, Bo; Gao, Chengyong; Gao, Liang; Gao, Qi; Gao, Wei; Ge, M. M.; Geng, L. S.; Gong, G.; Gou, Q. B.; Gu, M. H.; Guo, Fulai; Guo, J. G.; Guo, Xiaolei; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, Huihai; He, Junjiang; He, S. L.; He, Xinyu; He, Y.; Heller, M.; Hor, Y. K.; Hou, Chao; Hu, Haibing; Hu, S. C.; Hu, Xintian; Huang, Dezhi; Huang, Q.; Huang, Wenhao; Huang, X. T.; Huang, Xingtao; Huang, Z. C.; Ji, Fei; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin, Chao; Tang, Ke; Kuleshov, D.; Levochkin, K.; Li, B. B.; Liu, Cong; Li, Cheng; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.; Li, W. L.; Li, Xin; Li, X. R.; Li, Y.; Li, Y. Z.; Li, Zhe; Li, Zhuo; Liang, En‐Wei; Liang, Yun-Feng; Lin, S. J.; Liu, 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.; Long, W. J.; Lü, Rui; Lv, Hongkui; Q., B.; L., L.; H., X.; Mao, J.; Masood, A.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Qi, Y. Q.; Qiao, Bing-Qiang; Qin, Jiajun; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O. B.; Sheng, X. D.; Shi, J. Y.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.; Su, Yi‐Jiun; Sun, Q. N.; Sun, Xiao-Na; Sun, Zhang‐Hua; Tam, P. H. T.; Tang, Z.; Tian, Wei; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang, Longjun; 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; Wei, Da-Ming; Wei, J. J.; Wei, Y. J.; Wen, Tao; Wu, C. Y.; Wu, H. R.; Wu, Sha Sha; Wu, W. X.; Wu, X.; Xi, Shao-Qiang; Xia, J.; Xiang, G. M.; Xiao, D. X.; Xiao, G. C.; Xiao, H. B.; Xin, G. G.; Xin, Y.; Xing, Yongzhong; Xu, D. L.; Xu, Rong; Xue, L.; Yan, Dahai; Yan, Jun; Yang, Chaowen; Yang, Fang; Yang, Jian-Huan; Yang, L.; Yang, Mingjie; Yang, Rui; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, Na; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan, Qiang; Zeng, Houdun; Zeng, Tingxuan; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai, X. X.; Zhang, Bao-Tang; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang, J. W.; Zhang, Lu; Zhang, Li; Zhang, L. X.; 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, Yong; Zhang, Yi; Zhao, Bing; Zhao, Jing; Liu, Zhao; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, Bin; Zhou, H.; Zhou, J. N.; Zhou, Ping; Zhou, Rong; Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, Huibin; Zhu, K.; Zuo, Xin

doi:10.1103/physrevd.104.062007

Cited by 10 publications

(7 citation statements)

References 18 publications

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“…Unfortunately, for WFCTA this is not possible as at energy above few tens of TeV the geomagnetic field do not deflect anymore the CR. LHAASO managed, for the first time, to propagate the WCDA energy scales to WFCTA measurements through a set of commonly triggered events [18]. This overlap occurs in a limited energy range of WCDA-1, because the two detector have different energy thresholds.…”

Section: Cosmic Raysmentioning

confidence: 99%

Highlights from the Large High-Altitude Air-Shower Observatory (LHAASO)

Volpe¹

2023

J. Phys.: Conf. Ser.

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Since July 2021, LHAASO is fully operational and collecting data. The Nature paper in 2021, revealing 12 VHE new sources, was just the start of LHAASO science, revealing the huge scientific potential of this experiment. LHAASO opened the multi-TeV era in γ-ray astronomy and cosmic ray physics. Many analysis efforts in different areas are ongoing in different areas and several results are already published. In this contribution, we will show some highlights from LHAASO science together with the status of calibrations and performances achieved.

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Section: Cosmic Raysmentioning

confidence: 99%

Highlights from the Large High-Altitude Air-Shower Observatory (LHAASO)

Volpe¹

2023

J. Phys.: Conf. Ser.

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“…In such a setup, the scattered Cherenkov radiation could travel to neighbouring PMTs, blurring the response of the detector. In the HAWC [16] and LHAASO-WCDA [17] system, separate tanks or curtains were used to counteract such an effect. At a sufficiently high level above the energy threshold, the collection area of the gamma rays is closely related with the physical size of the array.…”

Section: Sa and Wcd Techniquesmentioning

confidence: 99%

TeV Instrumentation: Current and Future

Sitarek

2022

Galaxies

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During the last 20 years, TeV astronomy has turned from a fledgling field, with only a handful of sources, into a fully-developed astronomy discipline, broadening our knowledge on a variety of types of TeV gamma-ray sources. This progress has been mainly achieved due to the currently operating instruments: imaging atmospheric Cherenkov telescopes, surface arrays and water Cherenkov detectors. Moreover, we are at the brink of a next generation of instruments, with a considerable leap in performance parameters. This review summarizes the current status of the TeV astronomy instrumentation, mainly focusing on the comparison of the different types of instruments and analysis challenges, as well as providing an outlook into the future installations. The capabilities and limitations of different techniques of observations of TeV gamma rays are discussed, as well as synergies to other bands and messengers.

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“…In such a setup the scattered Cherenkov radiation could travel to neighbouring PMTs blurring the response of the detector. HAWC [16] and LHAASO-WCDA [17] use respectively separate tanks or curtains to counteract such an effect. Sufficiently high above the energy threshold, the collection area of the gamma rays is closely related with physical size of the array.…”

Section: Sa and Wcd Techniquementioning

confidence: 99%

TeV Instrumentation: current and future

Sitarek¹

2022

Preprint

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During the last 20 years, TeV astronomy turned from a fledgling field, with only a handful of sources into a fully-developed astronomy discipline, broadening our knowledge on a variety of types of TeV gamma-ray sources. This progress has been mainly achieved due to currently operating instruments: Imaging Atmospheric Cherenkov Telescopes, Surface Array and Water Cherenkov detectors. Moreover, we are at the brink of a next generation of instruments, with a considerable leap of performance parameters. This review summarises the current status of the TeV astronomy instrumentation, mainly focusing on the comparison of the different types of instruments and analysis challenges, as well as provides an outlook into the future installations. The capabilities and limitations of different techniques of observations of TeV gamma rays are discussed, as well as synergies to other bands and messengers.

show abstract

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

Cited by 10 publications

References 18 publications

Highlights from the Large High-Altitude Air-Shower Observatory (LHAASO)

Highlights from the Large High-Altitude Air-Shower Observatory (LHAASO)

TeV Instrumentation: Current and Future

TeV Instrumentation: current and future

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