当前引力波天文台在更高kHz、MHz和GHz频率下的光学灵敏度
Optical sensitivities of current gravitational wave observatories at higher kHz, MHz and GHz frequencies
AI总结：
本文计算了现有引力波天文台在kHz、MHz和GHz频段由光子散粒噪声主导的高频灵敏度，揭示其频率梳特性，为新型高频引力波探测器提供对比基准。
摘要：
GEO 600、Kagra、LIGO和Virgo的建造目的是观测音频频段内的引力波，因为此前预测该频段具有最高的事件率与最大的信噪比。目前，学界正在讨论可能在高频段产生信号的宇宙学起源假想源。尚不广为人知的是，当前的干涉式引力波天文台具有一个覆盖这些高频段的高光学灵敏度频率梳。本文在光子散粒噪声为主导噪声源的合理假设下，计算了正在运行的引力波天文台的高频噪声谱密度。我们解释了其背后的物理原理：当干涉仪臂不垂直于引力波传播方向时，对于天文台谐振腔自由光谱范围的所有整数倍频率，都能实现高灵敏度。新的高频引力波探测器概念提案必须与本文给出的高频灵敏度进行比较。
英文摘要：
GEO 600, Kagra, LIGO, and Virgo were built to observe gravitational waves at frequencies in the audio band, where the highest event rates combined with the largest signal to noise ratios had been predicted. Currently, hypothetical sources of cosmological origin that could have produced signals at higher frequencies are under discussion. What is not widely known is that current interferometric GW observatories have a frequency comb of high optical sensitivity that encompasses these high frequencies. Here we calculate the high-frequency noise spectral densities of operating GW observatories under the justified assumption that photon shot noise is the dominant noise source. We explain the underlying physics of why high sensitivity is achieved for all integer multiples of the free spectral ranges of the observatory's resonators when an interferometer arm is not orientated perpendicular to the propagation direction of the GW. Proposals for new concepts of high-frequency GW detectors must be compared with the high-frequency sensitivities presented here.
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