Comparative study of detection modes for space-based gravitational wave observation

Wu Jingui; Wang Xiaoyong; Bai Shaojun; Wu Kailan; Guo Zhongkai; Zheng Yongchao; Wang Yun; Lin Xuling

doi:10.12086/oee.2024.230134

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Wu J G, Wang X Y, Bai S J, et al. Comparative study of detection modes for space-based gravitational wave observation[J]. Opto-Electron Eng, 2024, 51(2): 230134. doi: 10.12086/oee.2024.230134

Citation:

Wu J G, Wang X Y, Bai S J, et al. Comparative study of detection modes for space-based gravitational wave observation[J]. Opto-Electron Eng, 2024, 51(2): 230134. doi: 10.12086/oee.2024.230134

Comparative study of detection modes for space-based gravitational wave observation

1.
Beijing Institute of Space Mechanics & Electricity, Beijing 100094, China
2.
School of Mathematical Science, Capital Normal University, Beijing 100048, China
3.
School of Physical Science and Technology, Lanzhou University, Lanzhou, Gansu 730000, China

Fund Project: Project supported by National Key Research and Development Program of China (2021YFC220144, 2021YFC2202102, 2020YFC2200404, 2020YFC2202201); Chinese Academy of Space Technology Outstanding Youth Fund (LXL2022); China Aerospace Science and Technology Corporation Youth Elite Talents Fund (201981)

More Information

Corresponding author: gezila@sina.cn

Received Date 12 June 2023

Revised Date 09 November 2023

Accepted Date 09 November 2023

Published Date 29 February 2024

Abstract

Abstract

In order to achieve the measurement of gravitational wave signals in the millihertz frequency band, the space-based gravitational wave detection projects such as LISA, TianQin, and Taiji projects, which are based on laser interference systems, require the hardware noise floor of the interferometers to be lower than the interstellar weak light shot noise limit. This imposes stringent engineering specifications on the optical-mechanical design and the corresponding interferometer payload. This paper approaches the issue from the perspective of detection mode selection and derives the expressions of readout noise and stray light noise in the interference signal under the single detector mode and the balanced mode. Furthermore, a detailed discussion is provided on the weak-light interference process of the scientific interferometer. The results demonstrate that the balanced mode is capable of suppressing the interference phase noise caused by laser power fluctuations and backscattered stray light across multiple orders of magnitude. However, the suppression capability is constrained by the unequal splitting property of the beam combiner. To address this, a relative gain factor is introduced to compensate for the unequal splitting property of the beam combiner. Further analysis reveals that electronic gain compensation can only eliminate the impact of unequal splitting on one of the two noises rather than both simultaneously. Therefore, a balance must be struck in selecting gain compensation between the suppression of laser power fluctuation noise and stray light noise. Even with this consideration, the balanced mode still offers significant noise suppression capabilities at a magnitude difference, thus potentially reducing the engineering requirements for laser power fluctuations and telescope backscattered stray light.
- gravitational wave observation /
- balanced detection mode /
- read out noise /
- straylight analysis

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References

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Overview

Overview

In order to achieve the measurement of gravitational wave signals in the millihertz frequency band, the space-based gravitational wave detection projects such as LISA, TianQin, and Taiji projects, which are based on laser interference systems, require the hardware noise floor of the interferometers to be lower than the interstellar weak light shot noise limit. This imposes stringent engineering specifications on the optical-mechanical design and the corresponding interferometer payload. This paper approaches the issue from the perspective of detection mode selection and derives the expressions of readout noise and stray light noise in the interference signal under the single detector mode and the balanced mode. Furthermore, a detailed discussion is provided on the weak-light interference process of the scientific interferometer. The results demonstrate that the balanced mode is capable of suppressing the interference phase noise caused by laser power fluctuations and backscattered stray light across multiple orders of magnitude. However, the suppression capability is constrained by the unequal splitting property of the beam combiner. To address this, a relative gain factor is introduced to compensate for the unequal splitting property of the beam combiner. Further analysis reveals that electronic gain compensation can only eliminate the impact of unequal splitting on one of the two noises rather than both simultaneously. Therefore, a balance must be struck in selecting gain compensation between the suppression of laser power fluctuation noise and stray light noise. Even with this consideration, the balanced mode still offers significant noise suppression capabilities at a magnitude difference, thus potentially reducing the engineering requirements for laser power fluctuations and telescope backscattered stray light.