High-Performance Telescope System Design for Space-Based Gravitational Waves Detection

被引:0
|
作者
Ji, Huiru [1 ,2 ,3 ]
Zhao, Lujia [1 ,2 ,3 ]
Fan, Zichao [1 ,2 ,3 ]
Fan, Rundong [4 ,5 ]
Cao, Jiamin [1 ,2 ,3 ]
Mo, Yan [1 ,2 ,3 ]
Tan, Hao [1 ,2 ,3 ]
Jiang, Zhiyu [1 ,2 ,3 ]
Ma, Donglin [1 ,2 ,3 ,4 ,5 ,6 ]
机构
[1] Huazhong Univ Sci & Technol, MOE Key Lab Fundamental Phys Quant Measurement, Wuhan 430074, Peoples R China
[2] Huazhong Univ Sci & Technol, Hubei Key Lab Gravitat & Quantum Phys, PGMF, Wuhan 430074, Peoples R China
[3] Huazhong Univ Sci & Technol, Sch Phys, Wuhan 430074, Peoples R China
[4] Huazhong Univ Sci & Technol, Sch Opt & Elect Informat, Wuhan 430074, Peoples R China
[5] Huazhong Univ Sci & Technol, Wuhan Natl Lab Optoelect, Wuhan 430074, Peoples R China
[6] Shenzhen Huazhong Univ Sci & Technol, Shenzhen 518057, Peoples R China
基金
中国国家自然科学基金; 国家重点研发计划;
关键词
gravitational waves detection; spaceborne telescope; optical system design; LISA; MISSION; ANTENNA;
D O I
10.3390/s24227309
中图分类号
O65 [分析化学];
学科分类号
070302 ; 081704 ;
摘要
Space-based gravitational wave (GW) detection employs the Michelson interferometry principle to construct ultra-long baseline laser interferometers in space for detecting GW signals with a frequency band of 10-4-1 Hz. The spaceborne telescope, as a core component directly integrated into the laser link, comes in various configurations, with the off-axis four-mirror design being the most prevalent. In this paper, we present a high-performance design based on this configuration, which exhibits a stable structure, ultra-low wavefront aberration, and high-level stray light suppression capabilities, effectively eliminating background noise. Also, a scientifically justified positioning of the entrance and exit pupils has been implemented, thereby paving adequate spatial provision for the integration of subsequent optical systems. The final design realizes a wavefront error of less than lambda/500 in the science field of view, and after tolerance allocation and Monte Carlo analysis, a wavefront error of less than lambda/30 can be achieved with a probability of 92%. The chief ray spot diagram dimensions are significantly small, indicating excellent control of pupil aberrations. Additionally, the tilt-to-length (TTL) noise and stray light meet the stringent requirements for space-based gravitational wave detection. The refined design presented in this paper proves to be a more fitting candidate for GW detection projects, offering more accurate and rational guidance.
引用
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页数:18
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