Search for High Energy Gamma-ray Sources in the Southern Sky

在南方天空寻找高能伽马射线源

基本信息

批准号：
02044079
负责人：
SATO Humitaka
金额：
$ 3.14万
依托单位：
Department of Physics, Kyoto University
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

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-02044079/
关键词：
Supernova SN1987A Ultra High Energy gamma-ray Counter Array Neutron Star Magellanic Cloud Ejecta SN 1987A 超高エネルギーガンマ線超新星1987A チェレンコフ光空気シャワーシンチレーション・カウンター・アレイ

项目摘要

The supernova 1987A in the Large Magellanic Cloud has provided the first opportunity to study the emission of particles and electromagnetic radiation from a young supernova. A rapidly rotating, magnetized neutron star at the center of the expanding ejecta may be a powerful source of ultra high-energy (UHE) cosmic rays. H. Sato has pointed out that high energy gamma-rays may be produced from the decay pions generated by the collisions of hadrons accelerated by the neutron star with supernova ejecta. We installed gamma-ray detectors at the Black Birch in New Zealand (1640 m above sea level, 41ﾟ45'S, 173ﾟ47'E). The counter array consists of 76 scintillation detectors. The observations started on 13 October 1987. An upper limit on tile flux of UHE gamma-rays from SN1987A (>100 TeV) was obtained to be 4X10^<-14> cm^<-2> sec^<-1> from the data of 1987-1991. gamma-rays above 3 TeV emitted by SN1987A have been searched for using three, Cerenkov mirrors and data give an upper bound on the flux of 5X10^<-12> cm^<-2> sec^<-1>. Data on January 14 and 15 1988 were found to have excess counts corresponding to a flux of (1.9<plus-minus>0.5)X10^<-11> cm^<-2> sec^<-1>. The observed time of the excess coincides with the time of X-ray flare detected by the Ginga Satellite.Recently, we have searched for UHE gamma-ray from Southern objects including Cen A, Vela X-1, Cen X-3, Cir X-1 and also several objects in the Magellanic Clouds. None of these sources shows significant excess events. The observation is still being carried out.The moon was used to measure the angular resolution of the detector through its shadowing effect. The density of the events at the center of the moon has been found to be lower than event density near direction of the moon.

大型麦哲伦云中的Supernova 1987a为研究了年轻的超新星的颗粒和电磁辐射的发射提供了第一个机会。在扩展的喷射中心的快速旋转，磁化的中子恒星可能是超高能量（UHE）宇宙射线的强大来源。 H. Sato指出，高能量伽马射线可能是由由中子恒星与超新星弹射器加速的Hadron产生的衰变产生的。我们在新西兰的黑桦树（海拔1640 m，41 ﾟ45，173 ﾟ47'e）安装了伽马射线探测器。计数器阵列由76个闪烁探测器组成。观察结果始于1987年10月13日。从1987-1991的数据中获得了SN1987A（> 100 tev）的UHE伽马射线的上限（> 100 TEV）为4x10^<-14> cm^<-2> sec^<-1>。 SN1987A发出的3个TEV以上的伽马射线已被搜索使用三个，Cerenkov镜子和数据，在5x10^<-12> CM^<-2> sec^<-1>的磁通上给出了上限。发现1988年1月14日和15号的数据超过了（1.9 <plus-minus> 0.5）x10^<-11> cm^<-2> sec^<-1>的通量。观察到的超过的时间与牙龈卫星检测到的X射线耀斑的时间一致。实际上，我们搜索了来自南部物体的UHE伽马射线，包括CEN A，CEN A，VELA X-1，CEN X-1，CEN X-3，CIR X-1，CIR X-1以及Magellanic Clouds中的几个对象。这些来源都没有显示出明显的超过事件。观察结果仍在进行。月亮通过其阴影效果来测量检测器的角度分辨率。发现它们在月球中心的事件的密度低于月球方向附近的事件密度。