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

• 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
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-08454060/
• 关键词: Gravitational Wave; Resonant-Mass Antenna; Cosmic Ray; Fabry=Perot Interferometer; 共鳴型重力波アンテナ; レーザートランスデスューサー

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.

本研究的目的是测量宇宙线入射时共振质量型引力波天线的激发。它将成为高灵敏度实验中引力波搜索的背景。共振质量引力波天线是安装在中国科学院宇宙线研究所的一个用于观测银河系超新星爆发引力波的仪器。它有一个高灵敏度的激光干涉传感器来检测质量激励。该系统由法布里-珀罗干涉仪组成，实现了探测器系统的稳定和高灵敏度工作。我们还为事件否决准备了宇宙射线计数器。由于宇宙线计数器的安装延迟，我们没有同时测量宇宙线否决系统和引力波天线的操作，但我们将在电子外围设备完成后开始同时操作。本研究中的传感器灵敏度为-10 <-17>m/nuHz。为了使工作稳定，我们监测法布里-珀罗腔的透射光强度。利用该反馈对转向镜进行调谐，并在在线数据采集系统中进行了真实的实时数据处理。该数据采集系统能够真实的实时显示分析结果，并实现了锁相放大器频率的在线调谐。如果可能的话，最好把热量计放在天线下面。然而，由于预算和场地的限制，我们使用塑料闪烁计数器与PMT（光电倍增管）。检查计数器，并在天线系统周围搭建设置框架，由于计数器系统延迟，我们没有测量天线的激励。然而，另一方面，我们在传感器开发方面获得了许多经验。

项目成果

N.Kanda et.al.: "Data Acquisition System for TAMA Gravitational Weve Interferometer" “Gravitational Weve Detection",Universal Academy Press.15-20 (1997)

N. Kanda 等人：“TAMA 引力波干涉仪数据采集系统”“引力波检测”，Universal Academy Press.15-20 (1997)

N.Kanda et al.: "Smith's algorithm as a fast trigger for TAMA" Proceedings of "Second Workshop on Gravitational Wave Data Analysis". EDITIONS FRONTIERES. 209-217 (1998)

N.Kanda 等人：“史密斯算法作为 TAMA 的快速触发”“第二届引力波数据分析研讨会”论文集。

N.Kanda et.al.: "Smith's algorithm as a fast trigger for TAMA" “Second Workshop on Gravitational Wave,Data Analysis",EDITIONS FRONTIERES. 209-217 (1998)

N.Kanda 等人：“史密斯算法作为 TAMA 的快速触发器”“第二次引力波数据分析研讨会”，EDITIONS FRONTIERES 209-217 (1998)。

N.Kanda et.al.: "Smith's algorithm as a fast trigger for TAMA" "Second Workshop on Gravitational Wave Data Analysis", EDITIONS FRONTIERES. 209-217 (1998)

N.Kanda 等人：“史密斯算法作为 TAMA 的快速触发器”“第二届引力波数据分析研讨会”，EDITIONS FRONTIERES。

N.Kanda et al.: "Data Acquisition System for TAMA Gravitational Wave Interferometer" Gravitational Wave Detection. Universal Academy Press. 15-20 (1997)

N.Kanda 等人：“TAMA 引力波干涉仪数据采集系统”引力波探测。