Observation of TeV Gamma-Ray Emissions from Supernova Remnants

超新星遗迹 TeV 伽马射线发射的观测

• 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
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-11304015/
• 关键词: High-energy-gamma-ray; Cherenkov Telescope; Cosmic Ray Origin; Air shower; Supernova Remnant; Shock Acceleration; チェレンコフ光望遠鏡; 空気シャワー; チェンレンコフ光望遠鏡

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年在南澳大利亚建造了10m Air Cherenkov望远镜来探索TeV伽马射线天体物理，并运行至今进行观测。在本项目中，我们主要进行了以下研究：（1）这一时期我们观测到了三颗超新星遗迹（SNR）：SN1006、RXJ1713和RCW86。我们再次确认了 SN1006 和 RXJ1713 的 TeV 伽马射线发射，这两个望远镜均使用我们之前的 3.8m 望远镜探测到了 TeV 伽马射线。 TeV区域附近获得的光谱表明，SN1006的TeV伽马射线发射可以用同步加速器-逆康普顿模型来解释，但RXJ1713的伽马射线发射似乎是由于SNR中加速质子产生的中性π介子的衰变所致。我们还检测到了RCW86的TeV伽马射线发射迹象，但还需要更多的观测来证实。(2)获得了伽马射线脉冲星PSR1706的TeV伽马射线发射谱，并且得到了大破断已观测到约 1 TeV。我们还分析了这颗脉冲星的钱德拉档案数据，获得了脉冲星及其星云的分离光谱。结合这些新数据，我们获得了该脉冲星云的多波长光谱，这显然表明TeV伽马射线发射不能用星云中激波终止区周围发生的同步加速器-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。 32通道ADC和前端模块是为了获取光电管的模拟信息而开发的，并于2001年安装。现在我们可以从所有512个光电管中获取定时和模拟信息。此外，数据采集系统也得到了改进，触发频率可以从20 Hz提高到80 Hz，死区时间为20%。

项目成果

H.Muraishi et al.: "Evidence for TeV gamma-ray emission from the shell type RNR RXJ1713.7-3946"Astronomy and Astrophysics. 354. L57-L61 (2000)

H.Muraishi 等人：“来自壳型 RNR RXJ1713.7-3946 的 TeV 伽马射线发射的证据”天文学和天体物理学。

R.Enomoto et al.: "The acceleration of cosmic-ray protons in the supernova remnant RXJ 1713.7-3946"Nature. 416. 823-826 (2002)

R.Enomoto 等人：“超新星遗迹 RXJ 1713.7-3946 中宇宙射线质子的加速”《自然》。

T. Tanimori, et al.: "Sub-TeV Gamma-Ray Astrophysics Using Large Air Cerenkov Telescope"Progress of Theoretical Physics Supplement. No.143. 78-98 (2001)

T. Tanimori 等人：“使用大型空气切伦科夫望远镜进行亚 TeV 伽马射线天体物理学”理论物理进展补充。

A.Kawachi,T.Tanimori et al.: "The Optical Reflector System for the CANGAROO-II Imaging Atmospheric Cherakor Telescope"Astroparticle Physics. 14. 261-269 (2001)

A.Kawachi、T.Tanimori 等人：“CANGAROO-II 成像大气 Cherakor 望远镜的光学反射器系统”天体粒子物理学。

H. Muraishi, et al.: "Evidence for TeV gamma-ray emission from the shell type SNR RX J1713.7-3946"Astronomy and Astrophysics. v.354. L57-L61 (2000)

H. Muraishi 等人：“来自壳型 SNR RX J1713.7-3946 的 TeV 伽马射线发射的证据”天文学和天体物理学。