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Proceedings Paper

The high energy cosmic-radiation detection (HERD) facility onboard China's Space Station
Author(s): S. N. Zhang; O. Adriani; S. Albergo; G. Ambrosi; Q. An; T. W. Bao; R. Battiston; X. J. Bi; Z. Cao; J. Y. Chai; J. Chang; G. M. Chen; Y. Chen; X. H. Cui; Z. G. Dai; R. D'Alessandro; Y. W. Dong; Y. Z. Fan; C. Q. Feng; H. Feng; Z. Y. Feng; X. H. Gao; F. Gargano; N. Giglietto; Q. B. Gou; Y. Q. Guo; B. L. Hu; H. B. Hu; H. H. He; G. S. Huang; J. Huang; Y. F. Huang; H. Li; L. Li; Y. G. Li; Z. Li; E. W. Liang; H. Liu; J. B. Liu; J. T. Liu; S. B. Liu; S. M. Liu; X. Liu; J. G. Lu; M. N. Mazziotta; N. Mori; S. Orsi; M. Pearce; M. Pohl; Z. Quan; F. Ryde; H. L. Shi; P. Spillantini; M. Su; J. C. Sun; X. L. Sun; Z. C. Tang; R. Walter; J. C. Wang; J. M. Wang; L. Wang; R. J. Wang; X. L. Wang; X. Y. Wang; Z. G. Wang; D. M. Wei; B. B. Wu; J. Wu; X. Wu; X. F. Wu; J. Q. Xia; H. L. Xiao; H. H. Xu; M. Xu; Z. Z. Xu; H. R. Yan; P. F. Yin; Y. W. Yu; Q. Yuan; M. Zha; L. Zhang; L. Zhang; L. Y. Zhang; Y. Zhang; Y. J. Zhang; Y. L. Zhang; Z. G. Zhao
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Paper Abstract

The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads of the cosmic lighthouse program onboard China's Space Station, which is planned for operation starting around 2020 for about 10 years. The main scientific objectives of HERD are indirect dark matter search, 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 104 cubes of LYSO crystals, corresponding to about 55 radiation lengths and 3 nuclear interaction lengths, respectively. The top STK microstrips of seven 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 SKTs 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, 20% for protons from 100 GeV to 1 PeV; electron/proton separation power better than 10-5; effective geometrical factors of >3 m2sr for electron and diffuse gamma-rays, >2 m2sr for cosmic ray nuclei. R and D is under way for reading out the LYSO signals with optical fiber coupled to image intensified CCD and the prototype of one layer of CALO.

Paper Details

Date Published: 31 July 2014
PDF: 9 pages
Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91440X (31 July 2014); doi: 10.1117/12.2055280
Show Author Affiliations
S. N. Zhang, Institute of High Energy Physics (China)
O. Adriani, INFN (Italy)
Univ. degli Studi di Firenze (Italy)
S. Albergo, INFN (Italy)
Univ. degli Studi di Catania (Italy)
G. Ambrosi, INFN (Italy)
Q. An, Univ. of Science and Technology of China (China)
T. W. Bao, Institute of High Energy Physics (China)
R. Battiston, INFN-TIFPA (Italy)
Univ. degli Studi di Trento (Italy)
X. J. Bi, Institute of High Energy Physics (China)
Z. Cao, Institute of High Energy Physics (China)
J. Y. Chai, Institute of High Energy Physics (China)
J. Chang, Purple Mountain Observatory (China)
G. M. Chen, Institute of High Energy Physics (China)
Y. Chen, Nanjing Univ. (China)
X. H. Cui, National Astronomical Observatories (China)
Z. G. Dai, Nanjing Univ. (China)
R. D'Alessandro, INFN (Italy)
Univ. degli Studi di Firenze (Italy)
Y. W. Dong, Institute of High Energy Physics (China)
Y. Z. Fan, Purple Mountain Observatory (China)
C. Q. Feng, Univ. of Science and Technology of China (China)
H. Feng, Tsinghua Univ. (China)
Z. Y. Feng, Institute of High Energy Physics (China)
X. H. Gao, Xi'an Institute of Optics and Precision Mechanics (China)
F. Gargano, INFN (Italy)
N. Giglietto, INFN (Italy)
Q. B. Gou, Institute of High Energy Physics (China)
Y. Q. Guo, Institute of High Energy Physics (China)
B. L. Hu, Xi'an Institute of Optics and Precision Mechanics (China)
H. B. Hu, Institute of High Energy Physics (China)
H. H. He, Institute of High Energy Physics (China)
G. S. Huang, Univ. of Science and Technology of China (China)
J. Huang, Institute of High Energy Physics (China)
Y. F. Huang, Nanjing Univ. (China)
H. Li, Institute of High Energy Physics (China)
L. Li, Institute of High Energy Physics (China)
Y. G. Li, Institute of High Energy Physics (China)
Z. Li, Peking Univ. (China)
E. W. Liang, Guangxi Univ. (China)
H. Liu, Institute of High Energy Physics (China)
J. B. Liu, Univ. of Science and Technology of China (China)
J. T. Liu, Institute of High Energy Physics (China)
S. B. Liu, Univ. of Science and Technology of China (China)
S. M. Liu, Purple Mountain Observatory (China)
X. Liu, Institute of High Energy Physics (China)
J. G. Lu, Institute of High Energy Physics (China)
M. N. Mazziotta, INFN (Italy)
N. Mori, INFN (Italy)
Univ. degli Studi di Firenze (Italy)
S. Orsi, ISDC Data Ctr. for Astrophysics, Univ. de Genève (Switzerland)
M. Pearce, KTH Royal Institute of Technology (Sweden)
M. Pohl, Univ. de Genève (Switzerland)
Z. Quan, Institute of High Energy Physics (China)
F. Ryde, KTH Royal Institute of Technology (Sweden)
H. L. Shi, Institute of High Energy Physics (China)
P. Spillantini, INFN (Italy)
Univ. degli Studi di Firenze (Italy)
M. Su, MIT Kavli Institute for Astrophysics and Space Research (United States)
Harvard-Smithsonian Cr. for Astrophysics (United States)
J. C. Sun, Institute of High Energy Physics (China)
X. L. Sun, Institute of High Energy Physics (China)
Z. C. Tang, Institute of High Energy Physics (China)
R. Walter, ISDC Data Ctr. for Astrophysics, Univ. de Genève (Switzerland)
J. C. Wang, Yunnan Astronomical Observatory (China)
J. M. Wang, Institute of High Energy Physics (China)
L. Wang, Xi'an Institute of Optics and Precision Mechanics (China)
R. J. Wang, Institute of High Energy Physics (China)
X. L. Wang, Univ. of Science and Technology of China (China)
X. Y. Wang, Nanjing Univ. (China)
Z. G. Wang, Institute of High Energy Physics (China)
D. M. Wei, Purple Mountain Observatory (China)
B. B. Wu, Institute of High Energy Physics (China)
J. Wu, China Univ. of Geosciences (China)
X. Wu, ISDC Data Ctr. for Astrophysics, Univ. de Genève (Switzerland)
X. F. Wu, Purple Mountain Observatory (China)
J. Q. Xia, Institute of High Energy Physics (China)
H. L. Xiao, Institute of High Energy Physics (China)
H. H. Xu, Institute of High Energy Physics (China)
M. Xu, Institute of High Energy Physics (China)
Z. Z. Xu, Univ. of Science and Technology of China (China)
H. R. Yan, Peking Univ. (China)
P. F. Yin, Institute of High Energy Physics (China)
Y. W. Yu, Central China Normal Univ. (China)
Q. Yuan, Institute of High Energy Physics (China)
M. Zha, Institute of High Energy Physics (China)
L. Zhang, Yunnan Univ. (China)
L. Zhang, Institute of High Energy Physics (China)
L. Y. Zhang, Institute of High Energy Physics (China)
Y. Zhang, Institute of High Energy Physics (China)
Y. J. Zhang, Institute of High Energy Physics (China)
Y. L. Zhang, Univ. of Science and Technology of China (China)
Z. G. Zhao, Univ. of Science and Technology of China (China)


Published in SPIE Proceedings Vol. 9144:
Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray
Tadayuki Takahashi; Jan-Willem A. den Herder; Mark Bautz, Editor(s)

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