Study of the Origin of Galactic Cosmic Ray using TeV gamma-ray imaging and spectra observed by CANGAROO-III

在此期间，我们建造了三个10米成像空气切伦科夫望远镜(IACT)，用于在南澳大利亚州的沃梅拉观测天体TeV伽马射线，并从2004年4月开始使用这三个望远镜进行立体观测。我们团队致力于这些望远镜的电子系统和在线系统的开发。特别是，在2004年12月，我们实现了立体观测的专用触发系统，其中至少有两个望远镜在大约1μ秒内探测到了流星雨。该系统使我们能够拒绝意外撞击和宇宙介子产生的背景触发，并获得稳定的运行。此外，我们还研究了夜空背景对利用闪光模拟数字化仪(FADC)进行成像分析的影响，FADC以500 MHz的采样率记录了光电倍增器的脉冲形状。通过这项研究，脉冲形状的精确测量有望提高强子簇射的角分辨率和抑制能力。我们还在CanGaroo(京都大学、东海大学和韩国大学)组织了分分析小组。用于独立分析。我们自主开发了立体观测的分析程序工具。使用这个程序，我们分析了几个SNR，SNR RXJ0852,1713和开普勒，以及两个脉冲星星云：CRAB和PSR1509。特别是，我们已经从RXJ0852获得了整个TeV伽马射线图像。我们还得到了开普勒的TeV伽马射线发射的上限。

In this period, we have constructed three 10m Imaging Air Cherenkov Telescopes (IACT) for the observation of celestial TeV gamma rays at Wommera in South Australia, and hegun the stereo observation using those three telescope since 2004 April. Our group made efforts to develop the electronics system and online system of these telescope. In particular, in 2004 December, we realized the specialized trigger system for the stereo observation in which at least two telescopes detects the shower within about 1 μsec. This system enables us to reject the background trigger generated by the accidental hits and cosmic muons, and to obtain the stable operation. In addition we have studied the effect of the night sky background to the imaging analysis using Flash Analog Digitizer (FADC), which records the pulse shapes of the photo-multiplier with the 500 MHz sampling rate. By this study, the precise measurement of the pulse shape is expected to improve the angular resolution and the rejection power of the hadron shower. Also we organized the sub-analysis team in the CANGAROO (Kyoto Univ., Tokai Univ., and Konan Univ.) for the independent analysis. We independently developed the analysis program tools for the stereo observation. Using this program we are analyzing the several SNRs, SNR RXJ0852, 1713, and Kepler, and two pulsar nebulae : Crab and PSR1509. In particular we have obtained the whole TeV gamma-ray image from RXJ0852. Also we have get the upper limit for the TeV gamma-ray emission from the Kepler.