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Progress in the research of testing and evaluation techniques for spaceborne gravitational wave telescopes
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摘要
在空间引力波探测任务中，星载望远镜承担太空超长干涉光路双向光束准直的重要作用。空间引力波探测对星载望远镜提出了pm级光程稳定性和低于10−10级后向杂散光水平的极高要求。超高水平指标要求超过了当前测试技术的精度极限，因此，针对星载望远镜发展测试与评估技术并开展系统超高精度测试是空间引力波探测计划成功的重要前提。本文在概述国内外在研的空间引力波探测星载望远镜研制情况的基础上，重点围绕星载望远镜的核心技术指标——光程稳定性和后向杂散光，介绍了在研望远镜的测试技术发展现状和已经取得的部分测试成果，以及各研究单位进一步的测试计划，为我国的空间引力波探测的星载望远镜测试与评估技术发展提供参考。
Abstract
Spaceborne telescopes for gravitational wave detection crucially collimate bidirectional beams in ultra-long interferometric optical paths. The faint optical path changes due to gravitational waves demand pm-level optical path length stability and below 10−10 level backscattered light in the telescopes. The ultra-high-level specifications requirements are out of state-of-the-art testing techniques. The development of testing and evaluation techniques for spaceborne telescopes is a crucial prerequisite for the success of the space gravitational wave detection program. This paper overviews the development of spaceborne gravitational wave detection telescopes, focusing on the optical path length stability and backscattered light testing status, results, and further plans, providing reference in the testing and evaluation of Chinese spaceborne gravitational wave detection telescopes.
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Overview
Overview: Gravitational waves are spacetime oscillations radiated outward by accelerating mass objects. Significant astronomical events in the universe, such as the merging of massive black holes, emit stronger gravitational waves. Detecting gravitational waves allows for a deeper study of the laws governing celestial bodies and the origins of the universe, making accurate detection crucial. Gravitational wave detection technology utilizes Michelson interferometers to convert the extremely faint spacetime fluctuations caused by gravitational waves into measurable changes in optical path length. Recently, ground-based large Michelson interferometers have achieved direct detection of high-frequency gravitational waves. However, the detection of low-frequency gravitational waves, which is equally important, is not feasible on the ground due to arm length and ground noise issues. This necessitates the construction of ultra-large Michelson interferometers in space for low-frequency gravitational wave detection. Spaceborne gravitational wave detection telescopes play a vital role in collimating bidirectional beams in ultra-long interferometric optical paths in space. The extremely subtle changes in optical path caused by gravitational waves impose high demands for pm-level optical path length stability and below 10−10 level backscattered light in these telescopes. The ultra-high level index requirements exceed the precision limits of current ground testing techniques for telescopes. To ensure that spaceborne telescopes maintain their ultra-high design performance in the orbital environment, developing testing and evaluation techniques for these key indicators is a crucial prerequisite for the success of the space gravitational wave detection program. This paper provides an overview of the development of spaceborne gravitational wave detection telescopes, both domestically and internationally. It focuses on the current status and some test results of optical path length stability and backscattered light testing of telescopes under development, as well as further testing plans, providing a reference for the testing and evaluation of Chinese space gravitational wave detection space-borne telescopes.
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图 5 空间引力波探测星载望远镜地面集成测试平台示意图
Figure 5. Space gravitational wave detection spaceborne telescope ground integrated test platform
图 9 Sang等基于光纤干涉仪的太极望远镜SiC框架稳定性测试装置。(a)光纤干涉仪位移测量原理；(b)测试平台示意图；(c)测试平台实物图[33]
Figure 9. Stability test of SiC frame of Taiji telescope based on fiber interferometer by Sang et al. (a) Principle of stability testing with fiber optic interferometer; (b) Schematic of the frame stability test platform; (c)Test platform pictures[33]
望远镜 口径 光程稳定性要求 杂散光要求 波前误差 指向偏差 LISA 30 cm $1 \;\mathrm{pm} / \mathrm{Hz}^{1 / 2} \times \displaystyle\sqrt {1 + { {\left( {\frac{ {3\;{\rm{m} }{\rm{H} }{\rm{z} } } }{f} } \right)}^4} }$ ＜10−10 ＜λ/30 10 nrad/Hz1/2 天琴 22 cm $\text{1}\;\text{pm/}{\text{Hz} }^{\text{1/2} }{@0.1\;{\rm{mHz}}-1\;{\rm{Hz}}}$ ＜10−10 ＜λ/30 — 太极 20 cm $\text{1}\;\text{pm}\text{/}{\text{Hz} }^{\text{1/2} }\text{×}\displaystyle\sqrt{\text{1+}{\left(\frac{\text{3}\;\text{mHz} }{ {f} }\right)}^{\text{4} } }$ ＜10−10 ＜λ/30 — 
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表 2 CFRP望远镜组件结构热机械要求与测试性能[47]
Table 2. CFRP telescope assembly structure thermo-mechanical requirements and tested performances[47]
Performance Requirement 1st test 2nd test 2nd test re-run CTE over 100 K/(1/K) ＜10−7 9.8×10−8 5.7×10−8 6.9×10−8 M1-M2 Longitudinal displacement dz/μm ＜5 −7.6 −8.5 −7.4 M1-M2 Lateral displacement dy/μm ＜2 (goal) −25.7 −26.3 −26.2 M1-M2 Rotation dRx/μrad ＜20 134.4 −57.3 −47.2
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