Observation of Very High Energy Gamma Rays with 7m telescope

1999年，也就是这个4年项目的最后一个财政年度，我们完成了7米口径望远镜各部分的调整，于1998年12月运到澳大利亚，并于1999年1月在南澳大利亚伍默拉观测点组装成7米口径的望远镜。继续3.8米望远镜的运行和数据分析。1998年6月，对7米望远镜的高方位角座进行了组装和操作，以确认其性能并测试驱动望远镜的软件程序。结果表明，望远镜的姿态控制在设计精度范围内。1998年7月至10月，我们对所有直径为80cm的球面反射镜进行了测试，确认其聚焦能力达到0.1°，然后在11月将这些反射镜安装到“支撑板”上。通过遥控驱动电机改变镜子的姿态，从而确保镜子的组装将在澳大利亚进行，不会出现意外问题。对光电倍增管和电子电路进行了测试，并开发了在线数据采集系统的软件程序。1999年1月，7米望远镜主体在澳大利亚观测点组装安装完毕。2月，电子电路连接到望远镜，3月开始测试望远镜的“整体”运行。我们继续发展3.8 m望远镜观测数据的分析技术，特别是利用切伦科夫光子的定时信息。将该技术应用于超新星遗迹SN 1006的数据，使我们能够获得该天体的微分能谱。

In the year of 1999, the last fiscal year of the present 4 years' project, we finalized adjustments of each part of the 7m aperture telescope, transported them to Australia in December 1998, and assembled them to construct a 7m telescope in the observation site in Woomera, South Australia in January 1999. We also continued operation and data-analysis of 3.8 m telescope.In June 1998, the altitute-azimuth mount of the 7m telescope was assembled and operated to confirm its performance and to test the software programs for driving the telescope. We found that the attitude of the telescope is controled with the designed accuracies.From July to October in 1998, we tested all the spherical mirrors of 80 cm diameter to confirm their focusing ability as good as 0.1° and then in November, these mirrors were installed onto the "support panel". The attitude of the mirrors was changed by using the driving motors of which movement is remote-controlled, the result ensuring that the assembling of the mirrors will be made in Australia with no unexpected problems.The test of photomultipliers and electronics circuits were made, as well as the development of the software program of on-line data taking system.In January 1999, the main body of the 7m telescope was assembled and installed in the observation site in Australia. In February, electronics circuits are connected to the telescope, aud the test "overall" operation of the telescope was commenced in March.We have continued development of the analysis technique of the observation data from the 3.8 m telescope, in particular by using the timing information of Cerenkov photons. The technique was applied to the data of the supernova remnant SN 1006, which enabled us to obtain the differential energy spectrum from the object.