High Energy Cosmic Ray Background for Resonant-Mass Gravitational Wave Antenna

谐振质量引力波天线的高能宇宙射线背景

基本信息

批准号：
08454060
负责人：
KANDA Nobuyuki
金额：
$ 3.84万
依托单位：
Miyagi University of Education (1997-1998)The University of Tokyo (1996)
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (B)
财政年份：
1996
资助国家：
日本
起止时间：
1996 至 1998
项目状态：
已结题

项目摘要

The aim of this research was a measurement of the excitation of the resonant-mass type gravitational wave antenna due to cosmic ray incident. It will become the background of the gravitational wave search in high sensitivity experiment. The resonant-mass gravitational wave antenna that is settled at institute of cosmic ray research is a monitor for the burst gravitational wave from supernova in our galaxy. It has a high sensitivity laser interferometric transducer to detect mass excitation. It consists of Fabry=Perot interferometer.In this research, we achieved stable and high sensitivity operation of the detector system. We also prepare the cosmic ray counters for incident veto. We did not measured cosmic ray veto system and gravitational wave antenna operation simultaneously, since an installation of the cosmic ray counter is delayed, however we will start simultaneous operation when the electronics peripherals will be completed.The sensitivity of the transducer is -10^<-17>m/nuHz in this research. To make the operation stable, we monitor an intensity of transmission light of Fabry=Perot cavity. The steering mirrors are tuned with this feedback.We made real time data processing in on-line data acquisition system. The data acquisition system shows the quick analysis result in real time, and it made possible to tune the lock-in amplifier frequency for phase sensitive measurement with on-line.For main purpose of this research, we preparing cosmic ray counter beyond the antenna. If possible, to place calorimeter under the antenna is best choice. However due to budget and site limitation, we use plastic scintillation counters with PMT(Photo Multiplier Tube). Counters are checked, and a frame for setting is constructed around the antenna system.Due to delay of counter system, we did not measure the excitation of the antenna. However, on the other hand, we got many experiences with transducer development.

这项研究的目的是测量由于宇宙射线入射而引起的谐振质量引力 - 引力天线。在高灵敏度实验中，它将成为重力波搜索的背景。在宇宙射线研究所定居的共振质量引力天线是我们银河系中超新星的爆发引力波的监测。它具有高灵敏度激光干涉透射率可检测质量激发。它由Fabry = Perot干涉仪组成。在这项研究中，我们实现了检测器系统的稳定和高灵敏度操作。我们还为事件否决权准备了宇宙射线柜台。我们没有同时测量宇宙射线否决系统和引力波天线的操作，因为宇宙射线计数器的安装延迟了，但是当电子外围设备将完成时，我们将开始同时操作。在这项研究中，transducer的敏感性为-10^<-17> m/nuHz。为了使操作稳定，我们监视Fabry = Perot腔的传输光强度。转向镜子通过此反馈调整。我们在在线数据采集系统中进行了实时数据处理。数据采集系统显示了实时的快速分析结果，并且可以使用在线进行锁定放大器频率进行锁定放大器频率。对于本研究的主要目的，我们准备了天线以外的宇宙射线计数器。如果可能的话，将热量表放在天线下是最佳选择。但是，由于预算和现场限制，我们使用PMT（照片乘数管）的塑料闪烁计数器。检查计数器，并在天线系统周围构建设置框架。延迟反系统，我们没有测量天线的激发。但是，另一方面，我们在传感器开发方面获得了许多经验。