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地基激光干涉引力波探测器不仅首次发现引力波、开创了一个观测天文学的全新分支—引力波天文学, 同时也是物理学相关领域前沿科学与先进技术的成功典范. 为了实现引力波探测的目标, 使引力波成为一个常态化的天文观测手段, 全球主要地基引力波探测器经历了持续数十年的技术升级与改造. 本文重点介绍LIGO、Virgo和KAGRA等探测器的升级历程, 详细分析了其关键技术改进, 包括激光功率增强、悬挂与隔振系统优化以及量子噪声抑制等方面进展. 这些技术进步显著提升了探测器在10至几千赫兹的灵敏度, 使其成功探测到数以百计的致密天体并合引力波信号. 展望未来, 第三代地基引力波探测器的建设将大幅度拓展引力波的探测能力, 为物理学和天文学研究开辟新的视野.Gravitational wave astronomy has rapidly developed into a powerful means of probing compact objects and understanding the evolution of the Universe. To improve sensitivity and extend the detection band, ground-based laser interferometers such as LIGO, Virgo, and KAGRA have undergone continuous upgrades. This review summarizes their systematic development with an emphasis on noise sources and mitigation strategies. After outlining the principle of gravitational wave detection with laser interferometry, we analyze dominant noise sources including quantum vacuum fluctuations, thermal noise, and seismic disturbances, and introduce techniques such as frequency-dependent squeezed light, advanced seismic isolation, multi-stage suspensions, and cryogenic mirrors. For LIGO, we highlight the transition from the Initial to Advanced configurations, which enabled strain sensitivities of the order of $10^{-24}/\sqrt{\text{Hz}}$ and led directly to the first detection GW150914 and over one hundred subsequent events during O1 to O4. The unique superattenuator system of Virgo and its recent implementation of squeezed light, as well as the underground design of KAGRA and the use of cryogenic sapphire test masses, represent different approaches to suppress low-frequency and thermal noise. In addition, we compare the technical routes adopted by different detectors and summarize the lessons learned from their upgrades, which provide valuable guidance for future detector designs. Finally, we present next-generation projects, including LIGO Voyager, the Cosmic Explorer and the Einstein Telescope, which aim to achieve up to orders of magnitude improvements in sensitivity and provide new research opportunities for gravitational-wave cosmology and fundamental physics. Overall, the evolution of detector technologies has been the key driver of progress in gravitational wave astronomy, and the forthcoming facilities will transform our ability to explore the Universe.
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Keywords:
- gravitational wave /
- laser interferometer /
- ground-based gravitational wave detection /
- astrophysics
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图 1 激光干涉引力波探测器简化结构图
Fig. 1. Simplified schematic diagram of a laser interferometric gravitational wave detector.
图 2 Advanced LIGO噪声灵敏度曲线由引力波探测器噪声计算器Gwinc给出. (https://git.ligo.org/gwinc/pygwinc)
Fig. 2. Advanced LIGO noise budget, given by gravitational wave interferometer noise calculator Gwinc (https://git.ligo.org/gwinc/pygwinc).
图 5 LIGO部分输入光学组件的悬挂系统[39]
Fig. 5. the suspension system of some input optical components of LIGO.
图 6 初代LIGO和Advanced LIGO应变灵敏度对比. 数据来源: https://gwosc.org/data/
Fig. 6. Strain Sensitivity Comparison between Initial LIGO and Advanced LIGO. Data sources: https://gwosc.org/data/
图 7 真空态光场与压缩真空态光场 (a) 真空态光场; (b) 压缩真空态光场
Fig. 7. Vacuum state and squeezed vacuum state of light: (a) vacuum; (b) squeezed.
图 8 LIGO Hanford在O4前调试期间的应变灵敏度曲线[19]
Fig. 8. Strain sensitivity of the LIGO Hanford measured during the pre-O4 commissioning phase.
图 13 各观测阶段不同引力波探测器的BNS范围
Fig. 13. BNS range of different gravitational wave detectors in various observing runs.
图 14 第二代与第三代引力波探测器应变灵敏度对比. 数据来源: https://git.ligo.org/gwinc/pygwinc, https://www.et-gw.eu/index.php/etsensitivities
Fig. 14. Comparison of sensitivity curves for second and third generation gravitational wave detectors. Data sources: https://git.ligo.org/gwinc/pygwinc, https://www.et-gw.eu/index.php/etsensitivities
表 1 初代LIGO(S1阶段)与Advanced LIGO的主要参数
Table 1. Key Parameters of Initial LIGO (S1 Phase) and Advanced LIGO.
参数 Initial LIGO (S1) Advanced LIGO 臂长 3995 m 3995 m 臂腔精细度 220 450 激光种类及波长 Nd:YAG, $ \lambda = 1064\ {\rm{nm}} $ Nd:YAG, $ \lambda = 1064\ {\rm{nm}} $ 功率循环镜处的输入功率 4.5 W 125 W 测试质量所用材料 熔融石英 熔融石英 测试质量尺寸及质量 直径25 cm, 厚度10 cm, 质量10.7 kg 直径34 cm, 厚度20 cm, 质量 40 kg 光束半径 ITM/ETM 3.9 cm / 4.5 cm 5.3 cm / 6.2 cm 输入清模器长度及精细度 24 m, 1350 32.9 m, 500 循环腔长度 PRC/SRC 9 m / - 57.6 m / 56.0 m 注1: ITM 表示输入测试质量, ETM 表示末端测试质量; PRC 为功率循环腔, SRC 为信号循环腔 
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