首页> 外文会议>American Society for Precision Engineering Topical Meeting on Control of Precision Systems >PROTOTYPING, TESTING AND PERFORMANCE OF THE TWO-STAGE SEISMIC ISOLATION SYSTEM FOR ADVANCED LIGO GRAVITATIONAL WAVE DETECTORS
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PROTOTYPING, TESTING AND PERFORMANCE OF THE TWO-STAGE SEISMIC ISOLATION SYSTEM FOR ADVANCED LIGO GRAVITATIONAL WAVE DETECTORS

机译:先进利极重力波检测器两级地震隔离系统的原型,测试和性能

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The goal of LIGO is to detect and analyze the gravitational waves produced by astrophysical events. LIGO consists of 4 km scale interferometric detectors located in Washington (LIGO Hanford Observatory, LHO) and Louisiana (LIGO Livingston Observatory, LLO). Gravitational waves appear as differential length changes in the perpendicular arms. To reach the required level of sensitivity (to motions of 10"18 m or less), the interferometer test masses must be isolated from several noise sources, including seismic motion, which is dominant at low frequencies. Initial LIGO has searched for signals, but none have yet been identified. A significant improvement in sensitivity is underway with the pending installation of Advanced LIGO (or aLIGO). Once running at full sensitivity, sources of gravitational are predicted to be regularly detected. A key element in this upgrade is the installation of extremely effective broadband seismic isolation and positioning systems. It will include, for every optic, three levels of isolation in series: an external (in air) active isolation and alignment stage with quiet-hydraulic actuators called HEPI, an internal (in vacuum) passive/active isolator called ISI (Internal Seismic Isolator) presented in this paper, and predominantly passive multiple pendulums to hold the optics. A multi-stage Internal Seismic Isolation platform will be used to support the beam splitter and each of the test mass optics. The platform should provide an isolation factor of 10 at 0.1 Hz and up to 2000 at 10 Hz. This active/passive system, called BSC-ISI, under development for several years, is made of two stages in series, each controlled in six degrees of freedom (DOF). This paper presents the prototyping, testing and current performance of the BSC-ISI system supporting a 920 kg total payload (370 kg of optical payload with the remaining 550 kg configured as ballast). In the next section, the BSC-ISI architecture and the prototype are presented. The active control strategy is presented in section 3. Initial performance results and related structural investigation are presented in section 4, followed by improved performance in section 5.
机译:Ligo的目标是检测和分析天体物理事件产生的引力波。 Ligo由4公里规模的干涉测量探测器组成,位于华盛顿(Ligo Hanford Indectatory,Lho)和路易斯安那州(Ligo Livingston天文台,LLO)。引力波出现在垂直臂中的差分长度变化。为了达到所需的灵敏度水平(对于10“或更低的运动),干涉仪测试质量必须从几个噪声源隔离,包括地震运动,这在低频下占主导地位。初始LIGO搜索了信号,但是尚未识别出来。敏感性的显着改善是在先进的Ligo(或Aligo)的待定安装中进行的。一旦以完全灵敏度运行,预计会定期检测到引力的源。这个升级中的一个关键元素是安装极其有效的宽带地震隔离和定位系统。它将包括,对于每种光学,串联三个隔离级别:外部(空中)主动隔离和对准阶段,具有典型的液压执行器,称为HEPI,内部(真空)本文呈现的被动/有源隔离器称为ISI(内部地震隔离器),主要是无源多个摆锤来保持光学器件。一个多级内部地震隔离平台将用于支撑分束器和每个测试质量光学器件。平台应在0.1Hz下提供100倍,最高可达200​​0倍。这种被称为BSC-ISI的主动/被动系统在开发工作几年中,由两个阶段串联制成,每个阶段都在六个自由(DOF)中受到控制。本文介绍了支持920公斤总有效载荷的BSC-ISI系统的原型,测试和电流性能(370千克光学有效载荷,其中剩余的550 kg配置为镇流器)。在下一节中,提出了BSC-ISI架构和原型。主动控制策略在第3节中提出。初始绩效结果和相关的结构调查在第4节中提出,其次是第5节的提高性能。

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