The All‐Particle Spectrum of Primary Cosmic Rays in the Wide Energy Range from 10<sup>14</sup>to 10<sup>17</sup>eV Observed with the Tibet‐III Air‐Shower Array

Amenomori, M.; Bi, X. J.; Chen, D.; Cui, S. W.; Danzengluobu,; Ding, L. K.; Ding, X. H.; Fan, Chao; Feng, C.; Feng, Z.; Feng, Z. Y.; Gao, X. Y.; Geng, Q. X.; Guo, H. W.; He, H. H.; He, M.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, Hongbo; Huang, J.; Huang, Q.; Jia, H. Y.; Kajino, F.; Kasahara, K.; Katayose, Y.; Kato, C.; Kawata, K.; Labaciren,; Le, G. M.; Li, A. F.; Li, J. Y.; Lou, Y.; Lü, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nakamura, Masaki; Ohnishi, M.; Ohta, I.; Onuma, H.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Saito, T.; Sakata, M.; Sako, T. K.; Shibata, M.; Shiomi, A.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; Tsuchiya, H.; Udo, S.; Wang, B.; Wang, H.; Wang, X.; Wang, Y.; Wang, Y. G.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yan, C. T.; Yang, X. C.; Yasue, S.; Ye, Z. H.; Yu, G. C.; Yuan, A. F.; Yuda, T.; Zhang, H. M.; Zhang, J. L.; Zhang, N. J.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhaxisangzhu,; Zhou, X. X.

doi:10.1086/529514

Cited by 207 publications

(187 citation statements)

References 29 publications

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“…For the primary cosmic rays, we examined three composition models, namely, "Hepoor", "He-rich" and "Gaisser-fit" models, in order to evaluate the systematic errors attributable to primary composition models. The "He-poor" model is based on the HD (Heavy Dominant) model mentioned in the paper [1], and it is slightly revised to match with the new all-particle energy spectrum [1], to be the new "He-poor" model. The "He-rich" model is the "Model B (a lightly harder spectrum than the previous on by taking account of the nonlinear effects)" mentioned in the paper [4].…”

Section: Monte Carlo Simulationmentioning

confidence: 99%

“…In all models mentioned above, each component is summed up so as to match with the all-particle spectrum with a sharp knee, which was obtained with the Tibet-III AS array [1]. Table 1 is a summary of the fractions of the components (P, He, Medium and Fe) of the three composition models in given energy regions for three primary models.…”

Section: Monte Carlo Simulationmentioning

confidence: 99%

“…The number of charged particles passing through the scintillator is defined as the PMT output (charge) divided by that of the single-particle peak. The single-particle peak is determined by a probe calibration [1,11] using cosmic rays, typically muons. The value of single-particle peak is measured as 1.98 MeV for YAC-I detectors and 6.28 MeV for the Tibet-III detectors.…”

Section: Monte Carlo Simulationmentioning

confidence: 99%

See 2 more Smart Citations

Sensitivity of YAC to measure the light-component spectrum of primary cosmic rays at the ‘knee’ energies

Zhai¹,

Huang²,

Chen³

et al. 2015

J. Phys. G: Nucl. Part. Phys.

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Abstract.A new air-shower core-detector array (YAC : Yangbajing Air-shower Core-detector array) has been developed to measure the primary cosmic-ray composition at the "knee" energies in Tibet, China, focusing mainly on the light components. The prototype experiment (YAC-I) consisting of 16 detectors has been constructed and operated at Yangbajing (4300 m a.s.l.) in Tibet since May 2009. YAC-I is installed in the Tibet-III AS array and operates together. In this paper, we performed a Monte Carlo simulation to check the sensitivity of YAC-I+Tibet-III array to the cosmic-ray light component of cosmic rays around the knee energies, taking account of the observation conditions of actual YAC-I+Tibet-III array. The selection of light component from others was made by use of an artificial neural network (ANN). The simulation shows that the light-component spectrum estimated by our methods can well reproduce the input ones within 10% error, and there will be about 30% systematic errors mostly induced by the primary and interaction models used. It is found that the full-scale YAC and the Tibet-III array is powerful to study the cosmic-ray composition, in particular, to obtain the energy spectra of protons and helium nuclei around the knee energies.PACS numbers: 98.70. Sa, 96.50.sb, 96.50.sd

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Section: Monte Carlo Simulationmentioning

confidence: 99%

Section: Monte Carlo Simulationmentioning

confidence: 99%

Section: Monte Carlo Simulationmentioning

confidence: 99%

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Sensitivity of YAC to measure the light-component spectrum of primary cosmic rays at the ‘knee’ energies

Zhai¹,

Huang²,

Chen³

et al. 2015

J. Phys. G: Nucl. Part. Phys.

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“…Extensions to the baseline design may be made to increase its effective geometrical factor for gamma-rays (and electrons) with excellent energy and angular resolution. [7]. The horizontal lines show the flux required above a certain energy for detecting 10 events in two years with different effective geometrical factor in units of m 2 sr.…”

Section: Herd Scientific Objectives Requirements and Baseline Designmentioning

confidence: 99%

“…Ground-based extensive air shower experiments [6,7,8] continue to make progress [9]; however, these experiments have difficulties in making composition-resolved high-energy resolution measurements of the fine structure of the "knee". On the other hand, experiments based on balloons [14,16], satellites [20], or the international space station [13] can measure the particle energy and charge directly; however, these experiments suffer from small geometrical factor and limited energy range to make statistically meaningful measurements of the "knee".…”

Section: Introductionmentioning

confidence: 99%

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Zhang¹,

Adriani²,

Albergo³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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PoS(ICRC2017)1077The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads onboard China's Space Station, which is planned for operation starting around 2025 for about 10 years. The main scientific objectives of HERD are searching for signals of dark matter annihilation products, precise cosmic electron (plus positron) spectrum and anisotropy measurements up to 10 TeV, precise cosmic ray spectrum and composition measurements up to the knee energy, and high energy gamma-ray monitoring and survey. HERD is composed of a 3-D cubic calorimeter (CALO) surrounded by microstrip silicon trackers (STKs) from five sides except the bottom. CALO is made of about 7,500 cubes of LYSO crystals, corresponding to about 55 radiation lengths and 3 nuclear interaction lengths, respectively. The top STK microstrips of six X-Y layers are sandwiched with tungsten converters to make precise directional measurements of incoming electrons and gamma-rays. In the baseline design, each of the four side STKs is made of only three layers microstrips. All STKs will also be used for measuring the charge and incoming directions of cosmic rays, as well as identifying back scattered tracks. With this design, HERD can achieve the following performance: energy resolution of 1% for electrons and gamma-rays beyond 100 GeV and 20% for protons from 100 GeV to 1 PeV; electron/proton separation power better than 10 −5 ; effective geometrical factors of >3 m 2 sr for electron and diffuse gamma-rays, >2 m 2 sr for cosmic ray nuclei. R&D is under way for reading out the LYSO signals with optical fiber coupled to image intensified IsCMOS and CALO prototype of 250 LYSO crystals.

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Cosmic Particle Accelerators

Hofmann¹,

Hinton²

2020

Particle Physics Reference Library

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In the century since the measurements of Victor Hess [1]—considered as the discovery of cosmic rays—the properties of cosmic rays, as they arrive on Earth, have been studied in remarkable detail; we know their energy spectrum, extending to 1020 eV, their elemental composition, their angular distribution, and we understand the basic energetic requirements of cosmic ray production in the Galaxy.

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The All‐Particle Spectrum of Primary Cosmic Rays in the Wide Energy Range from 10¹⁴to 10¹⁷eV Observed with the Tibet‐III Air‐Shower Array

Cited by 207 publications

References 29 publications

Sensitivity of YAC to measure the light-component spectrum of primary cosmic rays at the ‘knee’ energies

Sensitivity of YAC to measure the light-component spectrum of primary cosmic rays at the ‘knee’ energies

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Cosmic Particle Accelerators

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The All‐Particle Spectrum of Primary Cosmic Rays in the Wide Energy Range from 1014to 1017eV Observed with the Tibet‐III Air‐Shower Array

Cited by 207 publications

References 29 publications

Sensitivity of YAC to measure the light-component spectrum of primary cosmic rays at the ‘knee’ energies

Sensitivity of YAC to measure the light-component spectrum of primary cosmic rays at the ‘knee’ energies

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Cosmic Particle Accelerators

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Product

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The All‐Particle Spectrum of Primary Cosmic Rays in the Wide Energy Range from 10¹⁴to 10¹⁷eV Observed with the Tibet‐III Air‐Shower Array