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Zhang L Q, Zeng Y, Wu X H, et al. Progress in the research of testing and evaluation techniques for spaceborne gravitational wave telescopes[J]. Opto-Electron Eng, 2024, 51(2): 240027. doi: 10.12086/oee.2024.240027
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Progress in the research of testing and evaluation techniques for spaceborne gravitational wave telescopes
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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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References
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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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Zhang L Q, Zeng Y, Wu X H, et al. Progress in the research of testing and evaluation techniques for spaceborne gravitational wave telescopes[J]. Opto-Electron Eng, 2024, 51(2): 240027. doi: 10.12086/oee.2024.240027
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Figure 1.
Gravitational wave spectrum
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Figure 2.
Developing space gravitational wave detectors
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Figure 3.
Schematic diagram of space gravitational wave detectors. (a) Triangular constellation and six links of detectors; (b) Laser links between two spacecrafts[9]
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Figure 4.
Main research progress of spaceborne telescopes for gravitational wave detection[15-18,21-36]
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Figure 5.
Space gravitational wave detection spaceborne telescope ground integrated test platform
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Figure 6.
LISA telescope assembly dimensional stability test by Verlaan et al. (a) Schematic of TA’s length metrology platform; (b) Thermal vacuum test scheme[28,47]
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Figure 7.
Optical path length stability test of LISA telescope based on heterodyne interferometry at the University of Florida. (a) Schematic of optical path length stability test platform; (b) ULE proto-TTS[32]
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Figure 8.
TTS and dimension test result of ULE pTTS. (a) OptoCAD model of TTS; (b) Length noise test results of reference cavity and ULE pTTS and LISA requirement[32]
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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]
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Figure 10.
SiC frame dimensional stability test and numerical simulation results. (a) Power spectrum of room temperature environment test; (b) Power spectrum of in-orbit numerical simulation[33]
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Figure 11.
Dimensional stability test of Taiji telescope’s C/SiC support frame by Shen et al. (a) The thermal design of the test structure; (b) The multi-channel heterodyne interferometer test platform[34]
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Figure 12.
Schematic of the optical path length stability measurement scheme for the space gravitational wave detection spaceborne telescope[50]
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Figure 13.
Schematic of the coherent stray light detection based on the heterodyne interferometry[35]
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