Gravitational wave detection using laser interferometry beyond the standard quantum limit
Gravitational wave detection using laser interferometry beyond the standard quantum limit
复制标题
使用超出标准量子极限的激光干涉测量引力波
DOI：
10.1098/rsta.2017.0289
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发表时间：
2018
期刊：
影响因子：
--
通讯作者：
M. Heurs
中科院分区：
文献类型：
--
作者：
M. Heurs
干涉型引力波探测器(如先进的LIGO)使用高功率固态激光器，以最大限度地提高探测灵敏度，从而进入宇宙。这些复杂的光源在输出功率、发射频率和光束几何形状方面都是超稳定的；这是获得低探测器噪声的关键。然而，即使在技术上尽可能地降低所有激光噪声，激光不可避免的量子噪声仍然存在。这是作为量子力学基础的海森堡测不准原理的结果：在这种情况下，要同时将激光的相位噪声和幅度噪声降低到任意低的水平，从根本上是不可能的。这一事实在探测器噪声预算中表现为两个不同的噪声源--光子散粒噪声和量子辐射压力噪声--它们共同构成当前引力波探测器灵敏度的下限，这是干涉测量的标准量子极限。为了克服这一限制，提出了各种技术，其中包括非经典光的不同用途和可选的干涉仪拓扑。本文解释了量子噪声如何进入干涉型引力波探测器并在其中显现，并概述了为克服这一看似根本的限制而提出的一些方案，所有这些方案都是为了达到更高的引力波事件探测率的目标。本文是“引力波天文学的前景”讨论会的一部分。
Interferometric gravitational wave detectors (such as advanced LIGO) employ high-power solid-state lasers to maximize their detection sensitivity and hence their reach into the universe. These sophisticated light sources are ultra-stabilized with regard to output power, emission frequency and beam geometry; this is crucial to obtain low detector noise. However, even when all laser noise is reduced as far as technically possible, unavoidable quantum noise of the laser still remains. This is a consequence of the Heisenberg Uncertainty Principle, the basis of quantum mechanics: in this case, it is fundamentally impossible to simultaneously reduce both the phase noise and the amplitude noise of a laser to arbitrarily low levels. This fact manifests in the detector noise budget as two distinct noise sources—photon shot noise and quantum radiation pressure noise—which together form a lower boundary for current-day gravitational wave detector sensitivities, the standard quantum limit of interferometry. To overcome this limit, various techniques are being proposed, among them different uses of non-classical light and alternative interferometer topologies. This article explains how quantum noise enters and manifests in an interferometric gravitational wave detector, and gives an overview of some of the schemes proposed to overcome this seemingly fundamental limitation, all aimed at the goal of higher gravitational wave event detection rates. This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.
影响因子：
2.9
作者：
M. Wimmer;D. Steinmeyer;K. Hammerer;M. Heurs
通讯作者：
M. Wimmer;D. Steinmeyer;K. Hammerer;M. Heurs
影响因子：
8.6
作者：
Grote, H.;Danzmann, K.;Vahlbruch, H.
通讯作者：
Vahlbruch, H.
影响因子：
19.6
作者：
Ma, Yiqiu;Miao, Haixing;Chen, Yanbei
通讯作者：
Chen, Yanbei