The next detectors for gravitational wave astronomy
The next detectors for gravitational wave astronomy
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下一代引力波天文学探测器
DOI：
10.1007/s11433-015-5747-7
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发表时间：
2015-12
期刊：
影响因子：
--
通讯作者：
Page Michael
中科院分区：
文献类型：
--
作者：
Blair David;Ju Li;Zhao ChunNong;Wen LinQing;Miao Haixing;Cai RongGen;Gao JiangRui;Lin XueChun;Liu Dong;Wu Ling-An;Zhu ZongHong;Hammond Giles;Paik Ho Jung;Fafone Viviana;Rocchi Alessio;Blair Carl;Ma YiQiu;Qin JiaYi;Page Michael
本文着重介绍了在现有的地面探测器完成初始观测并可能实现第一次直接探测引力波之后，所需要的下一代引力波天文学探测器。下一代探测器将需要具有更高的灵敏度，同时使世界探测器阵列具有更高的角度分辨率，以实现信号源的定位。本文件第一节首先审查了关于下一代陆基探测器的提议，并对8公里臂长探测器的灵敏度进行了分析，该探测器被提议作为一种安全和经济有效的手段，将灵敏度提高4倍。强调了在中国和澳大利亚建立一对这样的探测器的科学益处。本文第二节讨论了测试质量的高性能悬浮系统，这将是未来探测器的关键部件，而第二节讨论了测试质量的高性能悬浮系统。3讨论了由作用在试验质量上的重力梯度力的涨落引起的牛顿噪声问题的解决方案。这样的引力扰动不能被屏蔽，除非进行测量和抑制，否则将限制在低频率灵敏度。教派。4和5涉及关键的业务技术，这些技术将是未来探测器的持续问题。第4节讨论了在室温下工作的所有高功率光功率干涉仪所需的热补偿系统的设计。参数不稳定性控制在第一节中讨论。5.直到最近才被证实出现在高级LIGO中的参数不稳定性现象，给未来的探测器带来了风险和机遇。未来探测器增强的途径将来自量子测量技术。第6节侧重于使用光学机械装置以获得更高的灵敏度，而第6节则侧重于使用光学机械装置来提高灵敏度。7回顾了一系列量子测量选项。
This paper focuses on the next detectors for gravitational wave astronomy which will be required after the current ground based detectors have completed their initial observations, and probably achieved the first direct detection of gravitational waves. The next detectors will need to have greater sensitivity, while also enabling the world array of detectors to have improved angular resolution to allow localisation of signal sources. Sect. 1 of this paper begins by reviewing proposals for the next ground based detectors, and presents an analysis of the sensitivity of an 8 km armlength detector, which is proposed as a safe and cost-effective means to attain a 4-fold improvement in sensitivity. The scientific benefits of creating a pair of such detectors in China and Australia is emphasised. Sect. 2 of this paper discusses the high performance suspension systems for test masses that will be an essential component for future detectors, while sect. 3 discusses solutions to the problem of Newtonian noise which arise from fluctuations in gravity gradient forces acting on test masses. Such gravitational perturbations cannot be shielded, and set limits to low frequency sensitivity unless measured and suppressed. Sects. 4 and 5 address critical operational technologies that will be ongoing issues in future detectors. Sect. 4 addresses the design of thermal compensation systems needed in all high optical power interferometers operating at room temperature. Parametric instability control is addressed in sect. 5. Only recently proven to occur in Advanced LIGO, parametric instability phenomenon brings both risks and opportunities for future detectors. The path to future enhancements of detectors will come from quantum measurement technologies. Sect. 6 focuses on the use of optomechanical devices for obtaining enhanced sensitivity, while sect. 7 reviews a range of quantum measurement options.
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影响因子：
5
作者：
J. Harms;Yanbei Chen;S. Chelkowski;A. Franzen;H. Vahlbruch;K. Danzmann;R. Schnabel
通讯作者：
J. Harms;Yanbei Chen;S. Chelkowski;A. Franzen;H. Vahlbruch;K. Danzmann;R. Schnabel
影响因子：
3.5
作者：
H. Miao;Huan Yang;R. Adhikari;Yanbei Chen
通讯作者：
H. Miao;Huan Yang;R. Adhikari;Yanbei Chen
影响因子：
8.6
作者：
Stephen Merkowitz
通讯作者：
Stephen Merkowitz
影响因子：
2.6
作者：
M. Evans;L. Barsotti;P. Fritschel
通讯作者：
M. Evans;L. Barsotti;P. Fritschel
影响因子：
5
作者：
A. Buonanno;Yanbei Chen;N. Mavalvala
通讯作者：
A. Buonanno;Yanbei Chen;N. Mavalvala