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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
Figure 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)
Figure 2. Advanced LIGO noise budget, given by gravitational wave interferometer noise calculator Gwinc (https://git.ligo.org/gwinc/pygwinc).
图 3 LIGO鸟瞰图[39]
Figure 3. Aerial view of LIGO.
图 4 LIGO激光系统中的环形振荡器[39]
Figure 4. the ring oscillator in the LIGO laser system.
图 5 LIGO部分输入光学组件的悬挂系统[39]
Figure 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/
Figure 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
Figure 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]
Figure 8. Strain sensitivity of the LIGO Hanford measured during the pre-O4 commissioning phase.
图 9 Virgo鸟瞰图[82]
Figure 9. Aerial view of Virgo.
图 10 Virgo采用的熔融石英材料的镜面悬挂丝[87]
Figure 10. Mirror suspension of fused silica fibers.
图 11 KAGRA鸟瞰图[95]
Figure 11. Aerial view of KAGRA.
图 12 KAGRA悬挂系统的示意图[99]
Figure 12. Schematic diagram of KAGRA suspension system.
图 13 各观测阶段不同引力波探测器的BNS范围
Figure 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
Figure 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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