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Development of High Energy Gamma Ray Telescope with High Angular Resolution and Observation of Gamma Ray Objects in the Southern Sky

高能高角分辨率伽马射线望远镜研制及南方天空伽马射线天体观测

基本信息

批准号：
02044034
负责人：
KIFUNE Tadashi
金额：
$ 8.64万
依托单位：
Institute for Cosmic Ray research
依托单位国家：
日本
项目类别：
Grant-in-Aid for international Scientific Research
财政年份：
1990
资助国家：
日本
起止时间：
1990 至 1991
项目状态：
已结题

项目摘要

An imaging Cerenkov telescope with an aperture of 3.8 m diameter started operation in January 1992 in South Australia. The telescope was brought to Australia at the beginning of 1991. After assembling the telescope, the focussing quality of mirror was checked by seeing a star image. The blur was less than 0.1ﾟ. The tracking accuracy was found as good as - <plus-minus>0.01ﾟ by seeing several stars in different directionThe phototube camera of the telescope has a small pixel size of 0.15ﾟ x 0.15ﾟ with a total field of view of about 2.5ﾟ diameter. The telescope, the first imaging telescope in the southern hemisphere, was aimed at the Vela Pulsar/nebula and Cen A during the period from January to March in 1992.The obtained data was analyzed to reconstruct Cerenkov images of cosmic ray particles. The general feature of the image appear consistent with what is expected from simulation calculation. A new thing about this imaging telescope is that the arrival time of photons in each phototube is measured. The background lights of night sky should have a uniform distribution of arrival time, which, experimentally proved by selecting the lights separated from a clustering signals of air shower image, will be useful to reduce the contamination of the background light in signal.Further analysis and continuing accumulation of data are to be done as well as improvements of observation technique, such as choosing the best way of making a trigger signal for lower energy threshold and constructing a camera of a wider field of view with a larger number of phototubes. The telescope is going to be used to achieve a simultaneous observation with the BIG RAT telescope of Adelaide University.

口径为 3.8 m 的切伦科夫成像望远镜于 1992 年 1 月在南澳大利亚开始运行。该望远镜于1991年初被带到澳大利亚。组装好望远镜后，通过观察星像来检查镜面的聚焦质量。模糊度小于0.1ﾟ。通过观察不同方向的几颗恒星，发现跟踪精度高达 - <正负>0.01ﾟ。望远镜的光电管相机的像素尺寸较小，为 0.15ﾟ x 0.15ﾟ，总视场直径约为 2.5ﾟ直径。该望远镜是南半球第一台成像望远镜，于1992年1月至3月期间瞄准船帆座脉冲星/星云和Cen A。对获得的数据进行分析，重建宇宙线粒子的切伦科夫图像。图像的总体特征与模拟计算的预期一致。这种成像望远镜的一个新特点是测量每个光电管中光子的到达时间。夜空背景光的到达时间应该是均匀分布的，通过选择从气簇图像的聚类信号中分离出来的光，实验证明这一点将有助于减少信号中背景光的污染。还需要进一步分析和不断积累数据，并改进观测技术，如选择较低能量阈值的最佳触发信号制作方式、构建具有更宽视场的相机等。更多数量的光电管。该望远镜将用于与阿德莱德大学的BIG RAT望远镜实现同步观测。