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Observation of TeV Gamma-Ray Emissions from Supernova Remnants

超新星遗迹 TeV 伽马射线发射的观测

基本信息

批准号：
11304015
负责人：
TANIMORI Toru
金额：
$ 18.2万
依托单位：
KYOTO UNIVERSITY (2000-2001)Tokyo Institute of Technology (1999)
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (A)
财政年份：
1999
资助国家：
日本
起止时间：
1999 至 2001
项目状态：
已结题

项目摘要

We have constructed the 10m Air Cherenkov telescope at South Australia to explore TeV gamma-ray astrophysics in 2000, and operated for the observation until now. In this project, we have studied mainly followings.(1) In this period we observed three Supernova Remnants(SNR), SN1006, RXJ1713, and RCW86. We have reconfirmed TeV gamma-ray emissions from SN1006 and RXJ1713 from both of which TeV gamma rays were detected using our previous 3.8m telescope. Obtained spectra around the TeV region indicates that TeV gamma-ray emission from SN1006 can be explained by the Synchrotron-inverse Compton model, but that from RXJ1713 seems due to the decay of neutral pion generated by accelerated protons in the SNR. Also we have detected the sign of TeV gamma-ray emission from RCW86, but we need more observation for the confirmation.(2) Spectrum of TeV gamma-ray emission from the gamma-ray pulsar PSR1706 have been obtained, and the large breaking of it around 1 TeV has been observed. Also we analyzed the Chandla archive data for this pulsar, and obtained the separated spectra of the pulsar and its nebula. Combined those new data, we obtained the multi-wavelength spectrum of this pulsar nebula, which obviously shows that TeV gamma-ray emission can not be explained by the synchrotron-inverse Compton process occurred around the shock terminated region in the nebula.(3) We increased the field of View of the camera by increasing additional 48 phototubes. 32-ch ADC and Front end module were developed for getting the analog information of phototubes, and installed in 2001. Now we can get both timing and analog information from all 512 phototubes. Also the data acquisition system has been improved, and then the trigger rate could be increased from 20 Hz to 80 Hz with 20% dead time.

我们于2000年在南澳建造了10米口径的切伦科夫望远镜，用于TeV γ射线天体物理探测，并一直运行至今。在本项目中，我们主要研究了以下内容。(1)在此期间，我们观测到三颗超新星遗迹（SNR），SN 1006，RXJ 1713和RCW 86。我们已经重新确认了来自SN 1006和RXJ 1713的TeV伽马射线发射，这两个TeV伽马射线都是使用我们以前的3.8米望远镜探测到的。在TeV附近获得的光谱表明，SN 1006的TeV γ射线发射可以用同步加速器逆康普顿模型来解释，但RXJ 1713的TeV γ射线发射似乎是由于SNR中加速质子产生的中性π介子的衰变。此外，我们还探测到了RCW 86的TeV γ射线发射信号，但我们需要更多的观测来确认。(2)获得了γ射线脉冲星PSR 1706的TeV γ射线发射谱，并观察到其在1 TeV附近的大破缺。分析了该脉冲星的光谱数据，得到了该脉冲星及其星云的分离光谱。结合这些新的数据，我们得到了该脉冲星星云的多波长光谱，这表明TeV γ射线辐射不能用星云激波终止区附近发生的同步逆康普顿过程来解释。(3)我们通过增加额外的48个光电管来增加相机的视野。2001年研制了32路模数转换器和前端模块，用于获取光电管的模拟信息。现在，我们可以从所有512个光电管中获得定时和模拟信息。对数据采集系统进行了改进，使触发频率从20 Hz提高到80 Hz，死区时间为20%。