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.
Design and Testing of a Prototype Pixellated CZT Detector and Shield for Hard X-Ray Astronomy
我们报告的设计和实验室测试的原型成像CZT探测器打算在2000年4月的气球飞行测试。该探测器测试了建造大面积CZT阵列所需的几项关键技术，这是拟议的硬X射线天文任务所需的。两个10 mm x 10 mm x 5 mm CZT探测器，每个探测器具有间距为2.5 mm的1.9 mm像素的4 x 4阵列，将以"倒装芯片“方式安装在印刷电路板载体卡上;探测器将以平铺配置相隔0.3 mm放置，以便在两个晶体上保持像素间距。一种探测器是eV Products高压布里奇曼CZT，另一种是IMARAD水平布里奇曼材料。两种检测器均由PC/104单板机控制的32通道VA-TA ASIC读出。由塑料闪烁体包围的无源屏蔽/准直器从五个侧面包围探测器，并提供约45度的视场。将该仪器记录的背景光谱与单元件CZT检测器（10 mm x 10 mm x 2 mm高压Bridgman材料，来自eV Products）测量的背景光谱进行比较，该检测器配有相同的无源/塑料准直器，但后部包括有源BGO屏蔽。这个探测器以前曾由我们飞行过，完全由一个被动的盖子屏蔽。我们描述了各种系统的初步实验室结果，讨论了初始背景模拟，并描述了我们的气球飞行试验计划。
Kinetic inductance detectors for millimeter and submillimeter astronomy / Détecteurs à inductance cinétique pour l'astronomie millimétrique et sub-millimétrique
我们提出了最近的发展动态电感探测器（KID）的大型阵列的探测器。主要应用是地基毫米波天文学。作为案例研究，我们特别关注我们自己的实验：NIKA（Néel IRAM KID阵列）。NIKA是目前使用KID仪器的最佳现场实验，包括为Pico Veleta的IRAM 30米望远镜设计的双波段成像系统。我们在这篇文章中描述，一般情况介绍后，KID的工作原理和读出电子，至关重要的是利用固有的KID多路复用。我们得出结论，在2010年10月举行的最后一次运行期间，NIKA在2 mm和1.4 mm处同时观察到的天文源的一个小子集。介绍了近年来有关电影电感探测大矩阵（KID）的研究成果，主要应用于太阳毫米波天文学。Nous détailons en particulier notre propre caméra：NIKA（Néel IRAM KID Arrays）qui est aujourd'hui l'instrument le plus abbatemettant en oeuvre des KID. NIKA是Pico Veleta的30米IRAM的双波段摄像机。通过对这些文字中的工具性背景的分析，我们解释了KIDS和演讲电子学的功能原理，这对于多路复用的潜在潜力至关重要。最后，我们提出了NIKA在2010年12月进行的2 mm和1.4 mm波段的观测结果。
