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The direct detection of gravitational waves has opened up a new window for understanding the universe and trailblazed multi-messenger astronomy. The frequency bands of gravitational waves generated by various astronomical events can cover a broadband range, and the detection mechanisms and schemes for gravitational waves in different frequency bands are different. For example, the ground-based gravitational wave detection has a frequency band ranging from 10 Hz to 10 kHz, which is based on Michelson interferometer. The space gravitational wave detection has a frequency band in a range of 0.1 mHz–1 Hz , which is based on space interferometer. The pulsar gravitational wave detection has a frequency band ranging from 1×10–9 Hz to 1×10–7 Hz, which is based on pulsar timing array. The next-generation ground-based gravitational wave project requires higher sensitivity to detect faint signals, necessitating an assessment system with minimal background noise to accurately measure the laser relative intensity noise. At present, the detection frequency band of ground-based gravitational wave detection devices in operation is mainly concentrated in a range of 10 Hz–10 kHz. To satisfy the detection sensitivity requirements, the laser relative intensity noise should be accurately evaluated and suppressed to ≤2.0×10–9 Hz–1/2 at 10 Hz and ≤4.0×10–7 Hz–1/2 at 10 kHz by photoelectric feedback. In this work, an evaluation and characterization system is constructed for ground-based gravitational wave band laser intensity noise, which is based on low noise and high sensitivity photoelectric detection device and combined with LabVIEW and MATLAB algorithm programming for instrument control and data processing. This low noise evaluation system is used to test the background noise of fast Fourier transform (FFT) analyzer SR760, preamplifier SR560, photoelectric detector electronic noise and intensity noise of homemade optical fiber amplifier, and then the data extraction and image processing are carried out by LabVIEW and MATLAB algorithms, and finally the ground-based gravitational wave frequency band system is evaluated. The experimental results show that the electronic noises for the preamplifier SR560 and the FFT analyzer SR760 are lower than 3.8×10–9 Hz–1/2@(10 Hz–10 kHz). The electronic noise for the photodetector is lower than $ 1.4 \times {10^{ - 8}}\;{\text{V}}/\sqrt {{\text{Hz}}} $ at 10 Hz and $ 8.1 \times {10^{ - 9}}\;{\text{V}}/\sqrt {{\text{Hz}}} $ at 10 kHz, and the accuracy of the system is calibrated and tested by the standard sinusoidal signal. Finally, the noise of commercial laser is evaluated and compared with the factory data to verify the accuracy of the evaluation system. Related research, device and system development provide hardware, software and theoretical basis for preparing high-power low-noise laser light source and gravitational wave detection, and also provide the theoretical basis and evaluation criteria for detecting the ground-based gravitational wave .
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Keywords:
- laser intensity noise evaluation system /
- gravitational wave detection /
- low-noise laser source /
- low-noise photodetector
[1] Sathyaprakash B S, Schutz B F 2009 Living Rev. Relativ. 12 2
Google Scholar
[2] Schmidt P 2019 J. Phys. Conf. Ser. 1468 012218
Google Scholar
[3] Patrick K 2010 Ph. D. Dissertation (Hannover: Vom Fachbereich Physik der Universiät Hannover
[4] Anza S 2005 Classical Quant. Grav. 22 S125
Google Scholar
[5] Rer N 2005 Ph. D Dissertation (Hannover: Vom Fachbereich Physik der Universiät Hannover
[6] Armano M, et al. (LIGO Scientific and Virgo Collaboration) 2016 Phys. Rev. Lett. 116 231101
Google Scholar
[7] 王在渊, 王洁浩, 李宇航, 柳强 2023 物理学报 72 054205
Google Scholar
Wang Z Y, Wang J H, Li Y H, Liu Q 2023 Acta Phys. Sin. 72 054205
Google Scholar
[8] Ran D 2024 J. Cosmol. Astropart. Phys. 2 16
Google Scholar
[9] Daniel J, Andrew Z, Ryan M, Valentina D 2022 Astrophys. J. Lett. 1 L7
Google Scholar
[10] Abbott B P, et al. (LIGO Scientific and Virgo Collaboration) 2016 Phys. Rev. Lett. 116 061102
Google Scholar
[11] Antonino C 2023 EPJ Web of Conferences RICAP-22 280 03003
Google Scholar
[12] Hofacker C 2020 Aerospace Am. 58 10
[13] 李庆回, 李卫, 孙瑜, 王雅君, 田龙, 陈力荣, 张鹏飞, 郑耀辉 2022 物理学报 71 164203
Google Scholar
Li Q H, Li W, Sun Y, Wang Y J, Tian L, Chen L R, Zhang P F, Zheng Y H 2022 Acta Phys. Sin. 71 164203
Google Scholar
[14] 李卫, 谢超帮, 李庆回, 鞠明健, 武志学, 郑耀辉 2023 量子光学学报 29 040201
Google Scholar
Li W, Xie C B, Li Q H, Ju M J, Wu Z X, Zheng Y H 2023 J. Quantum Optics 29 040201
Google Scholar
[15] Gao L, Zheng L A, Lu B, Shi S P, Tian L, Zheng Y H 2024 Light Sci. Appl. 13 294
Google Scholar
[16] 郭禧庆, 周静, 王晨曦, 秦琛, 郭成哲, 李刚, 张鹏飞, 张天才 2024 物理学报 73 050401
Google Scholar
Guo X Q, Zhou J, Wang C X, Qin C, Guo C Z, Li G, Zhang P F, Zhang T C 2024 Acta Phys. Sin. 73 050401
Google Scholar
[17] Vahlbruch H, Wilken D, Mehmet M 2018 Phys. Rev. Lett. 121 173601
Google Scholar
[18] Acernese F, Agathos M. 2019 Phys. Rev. Lett. 123 2311081
Google Scholar
[19] Benno W, Peter K, Rick S, Peter F 2011 Pre-Stabilized Laser Design Requirements LIGO-T050036-v4
[20] Rollins J, Ottaway D, Zucker M, Weiss R, Abbott R 2004 Opt. Lett. 29 1876
Google Scholar
[21] Patrick K, Benno W, Karsten D 2009 Opt. Lett. 34 2912
Google Scholar
[22] Jonas J, Patrick O, Benno W 2017 Opt. Lett. 42 755
Google Scholar
[23] 李番, 王嘉伟, 高子超, 李健博, 安炳南, 李瑞鑫, 白禹, 尹王保, 田龙, 郑耀辉 2022 物理学报 71 209501
Google Scholar
Li F, Wang J W, Gao Z C, Li J B, An B N, Li R X, Bai Y, Yin W B, Tian L, Zheng Y 2022 Acta Phys. Sin. 71 209501
Google Scholar
[24] Michael T, Gerhard H 2006 Measurement 39 12
Google Scholar
[25] Fabian M, Benno W 2022 Instruments 15 1
Google Scholar
[26] Cooley J W, Tukey J W 1965 Math. Comput. 19 297
Google Scholar
[27] Welch P D 1967 IEEE Trans. Audio Electroacoust. 15 70
Google Scholar
[28] 张骥, 魏珊珊, 刘昊炜, 刘元煌, 姚波, 毛庆和 2021 中国激光 48 0301002
Google Scholar
Zhang J, Wei S S, Liu H W, Liu Y H, Yao B, Mao Q H 2021 Chin. J. Lasers 48 0301002
Google Scholar
[29] 郑立昂, 李番, 王嘉伟, 李健博, 高丽, 贺子洋, 尚鑫, 尹王保, 田龙, 杨文海, 郑耀辉 2023 光学学报 52 0552220
Google Scholar
Zheng L A, Li F, Wang J W, Li J B, Gao L, He Z Y, Shang X, Yin W B, Tian L, Yang W H, Zheng Y H 2023 Acta Photonica Sin. 52 0552220
Google Scholar
[30] Goßler S, Bertolini A, Born M, Chen Y, Dahl K, Gering D, Gräf C, Heinzel G, Hild S, Kawazoe F, Kranz O, Kühn G, Lück H, Mossavi K, Schnabel R, Somiya K, Strain K A, Taylor J R, Wanner A, Westphal T, Willke B, Danzmann K 2010 Classical Quant. Grav. 27 084023
Google Scholar
[31] Patrick K, Frank S, Benno W, Karsten D 2007 Rev. Sci. Instrum. 78 073103
Google Scholar
[32] Frank S, Patrick K, Michèle H, Benno W, Karsten D 2006 Opt. Lett. 13 2000
Google Scholar
[33] Jennrich O, Newton G, Skeldon K D, Hough J 2002 Opt. Com. 205 405
Google Scholar
[34] 刘骏杨, 韩逸凡, 陈力荣, 赵琴, 武延鹏, 李林, 王雅君, 郑耀辉 2025 量子光学学报 31 040201
Google Scholar
Liu J Y, Han Y F, Chen L R, Zhao Q, Wu Y P, Li L, Wang Y J, Zheng Y H 2025 J. Quantum Opt. 31 040201
Google Scholar
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图 1 地基引力波探测频段激光强度噪声测试评估系统架构
Figure 1. Architecture of laser intensity noise measurement and evaluation system.
图 2 地基引力波探测频段激光强度噪声评估系统程序流程图
Figure 2. Program flow chart of laser intensity noise evaluation system for ground-based GW detection.
图 4 高精度测试仪器本底噪声表征 (a) FFT分析仪测试结果; (b)外加前置放大器后电子学噪声测试结果
Figure 4. Electronic noise characterization of high precision instruments: (a) The test result of FFT; (b) the electronic noise characterization of pre-amplifier.
图 3 地基引力波探测频段激光强度噪声评估系统实验装置示意图, 其中Laser为激光器; ISO为光隔离器; λ/4为λ/4波片; λ/2为λ/2波片; PBS为偏振分束棱镜; BS为分束棱镜; len为f = 50 mm透镜; PD为光电探测器; PA为前置放大器; FFT analyzer为傅里叶分析仪; OSC为示波器; Vref为参考电压源; PC为计算机
Figure 3. Evaluation system for laser intensity noise at ground-based gravitational wave detection frequency band, where Laser is soild state laser, ISO is isolator, λ/4 is λ/4 waveplate, λ/2 is λ/2 waveplate, PBS is polarization beam splitter, BS is beam splitter, len is f = 50 mm len, PD is photodetector, PA is pre-amplifier, FFT analyzer is SR760, OSC is oscilloscope, Vref is voltage reference, PC is computer.
图 5 信号源验证结果
Figure 5. Verification results with 1 mV sinusoidal signal.
图 6 (a)光电探测器原理图; (b)不同探测器性能对比测试
Figure 6. (a) Schematic diagram of PD; (b) the contrast test of different PD’s performance.
图 7 不同商用激光器输出激光相对强度噪声测试结果
Figure 7. Test relative intensity noise results of different commercial lasers.
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[1] Sathyaprakash B S, Schutz B F 2009 Living Rev. Relativ. 12 2
Google Scholar
[2] Schmidt P 2019 J. Phys. Conf. Ser. 1468 012218
Google Scholar
[3] Patrick K 2010 Ph. D. Dissertation (Hannover: Vom Fachbereich Physik der Universiät Hannover
[4] Anza S 2005 Classical Quant. Grav. 22 S125
Google Scholar
[5] Rer N 2005 Ph. D Dissertation (Hannover: Vom Fachbereich Physik der Universiät Hannover
[6] Armano M, et al. (LIGO Scientific and Virgo Collaboration) 2016 Phys. Rev. Lett. 116 231101
Google Scholar
[7] 王在渊, 王洁浩, 李宇航, 柳强 2023 物理学报 72 054205
Google Scholar
Wang Z Y, Wang J H, Li Y H, Liu Q 2023 Acta Phys. Sin. 72 054205
Google Scholar
[8] Ran D 2024 J. Cosmol. Astropart. Phys. 2 16
Google Scholar
[9] Daniel J, Andrew Z, Ryan M, Valentina D 2022 Astrophys. J. Lett. 1 L7
Google Scholar
[10] Abbott B P, et al. (LIGO Scientific and Virgo Collaboration) 2016 Phys. Rev. Lett. 116 061102
Google Scholar
[11] Antonino C 2023 EPJ Web of Conferences RICAP-22 280 03003
Google Scholar
[12] Hofacker C 2020 Aerospace Am. 58 10
[13] 李庆回, 李卫, 孙瑜, 王雅君, 田龙, 陈力荣, 张鹏飞, 郑耀辉 2022 物理学报 71 164203
Google Scholar
Li Q H, Li W, Sun Y, Wang Y J, Tian L, Chen L R, Zhang P F, Zheng Y H 2022 Acta Phys. Sin. 71 164203
Google Scholar
[14] 李卫, 谢超帮, 李庆回, 鞠明健, 武志学, 郑耀辉 2023 量子光学学报 29 040201
Google Scholar
Li W, Xie C B, Li Q H, Ju M J, Wu Z X, Zheng Y H 2023 J. Quantum Optics 29 040201
Google Scholar
[15] Gao L, Zheng L A, Lu B, Shi S P, Tian L, Zheng Y H 2024 Light Sci. Appl. 13 294
Google Scholar
[16] 郭禧庆, 周静, 王晨曦, 秦琛, 郭成哲, 李刚, 张鹏飞, 张天才 2024 物理学报 73 050401
Google Scholar
Guo X Q, Zhou J, Wang C X, Qin C, Guo C Z, Li G, Zhang P F, Zhang T C 2024 Acta Phys. Sin. 73 050401
Google Scholar
[17] Vahlbruch H, Wilken D, Mehmet M 2018 Phys. Rev. Lett. 121 173601
Google Scholar
[18] Acernese F, Agathos M. 2019 Phys. Rev. Lett. 123 2311081
Google Scholar
[19] Benno W, Peter K, Rick S, Peter F 2011 Pre-Stabilized Laser Design Requirements LIGO-T050036-v4
[20] Rollins J, Ottaway D, Zucker M, Weiss R, Abbott R 2004 Opt. Lett. 29 1876
Google Scholar
[21] Patrick K, Benno W, Karsten D 2009 Opt. Lett. 34 2912
Google Scholar
[22] Jonas J, Patrick O, Benno W 2017 Opt. Lett. 42 755
Google Scholar
[23] 李番, 王嘉伟, 高子超, 李健博, 安炳南, 李瑞鑫, 白禹, 尹王保, 田龙, 郑耀辉 2022 物理学报 71 209501
Google Scholar
Li F, Wang J W, Gao Z C, Li J B, An B N, Li R X, Bai Y, Yin W B, Tian L, Zheng Y 2022 Acta Phys. Sin. 71 209501
Google Scholar
[24] Michael T, Gerhard H 2006 Measurement 39 12
Google Scholar
[25] Fabian M, Benno W 2022 Instruments 15 1
Google Scholar
[26] Cooley J W, Tukey J W 1965 Math. Comput. 19 297
Google Scholar
[27] Welch P D 1967 IEEE Trans. Audio Electroacoust. 15 70
Google Scholar
[28] 张骥, 魏珊珊, 刘昊炜, 刘元煌, 姚波, 毛庆和 2021 中国激光 48 0301002
Google Scholar
Zhang J, Wei S S, Liu H W, Liu Y H, Yao B, Mao Q H 2021 Chin. J. Lasers 48 0301002
Google Scholar
[29] 郑立昂, 李番, 王嘉伟, 李健博, 高丽, 贺子洋, 尚鑫, 尹王保, 田龙, 杨文海, 郑耀辉 2023 光学学报 52 0552220
Google Scholar
Zheng L A, Li F, Wang J W, Li J B, Gao L, He Z Y, Shang X, Yin W B, Tian L, Yang W H, Zheng Y H 2023 Acta Photonica Sin. 52 0552220
Google Scholar
[30] Goßler S, Bertolini A, Born M, Chen Y, Dahl K, Gering D, Gräf C, Heinzel G, Hild S, Kawazoe F, Kranz O, Kühn G, Lück H, Mossavi K, Schnabel R, Somiya K, Strain K A, Taylor J R, Wanner A, Westphal T, Willke B, Danzmann K 2010 Classical Quant. Grav. 27 084023
Google Scholar
[31] Patrick K, Frank S, Benno W, Karsten D 2007 Rev. Sci. Instrum. 78 073103
Google Scholar
[32] Frank S, Patrick K, Michèle H, Benno W, Karsten D 2006 Opt. Lett. 13 2000
Google Scholar
[33] Jennrich O, Newton G, Skeldon K D, Hough J 2002 Opt. Com. 205 405
Google Scholar
[34] 刘骏杨, 韩逸凡, 陈力荣, 赵琴, 武延鹏, 李林, 王雅君, 郑耀辉 2025 量子光学学报 31 040201
Google Scholar
Liu J Y, Han Y F, Chen L R, Zhao Q, Wu Y P, Li L, Wang Y J, Zheng Y H 2025 J. Quantum Opt. 31 040201
Google Scholar
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