Observation of Multi-TeV Gamma Rays from the Crab Nebula using the Tibet Air Shower Array
Observation of Multi-TeV Gamma Rays from the Crab Nebula using the Tibet Air Shower Array
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DOI：
10.1086/312342
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发表时间：
1999-09
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通讯作者：
M. Amenomori;S. Ayabe;P. Cao;Danzengluobu;L. Ding;Z. Feng;Y. Fu;H. Guo;M. He;K. Hibino;N. Hotta;Q. Huang;A. Huo;K. Izu;H. Jia;F. Kajino;K. Kasahara;Y. Katayose;Labaciren;J. Li;H. Lu;S. L. Lu;G. Luo;X. Meng;K. Mizutani;J. Mu;H. Nanjo;M. Nishizawa;M. Ohnishi;I. Ohta;T. Ouchi;J. Ren;T. Saito;M. Sakata;T. Sasaki;Z. Shi;M. Shibata;A. Shiomi;T. Shirai;H. Sugimoto;K. Taira;Y. Tan;N. Tateyama;S. Torii;T. Utsugi;C. Wang;H. Wang;X. W. Xu;Y. Yamamoto;G. Yu;A. Yuan;T. Yuda;C. S. Zhang;H. Zhang;J. Zhang;N. Zhang;X. Zhang;Zhaxisangzhu;Zhaxiciren;W. Zhou
中科院分区：
文献类型：
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作者：
M. Amenomori;S. Ayabe;P. Cao;Danzengluobu;L. Ding;Z. Feng;Y. Fu;H. Guo;M. He;K. Hibino;N. Hotta;Q. Huang;A. Huo;K. Izu;H. Jia;F. Kajino;K. Kasahara;Y. Katayose;Labaciren;J. Li;H. Lu;S. L. Lu;G. Luo;X. Meng;K. Mizutani;J. Mu;H. Nanjo;M. Nishizawa;M. Ohnishi;I. Ohta;T. Ouchi;J. Ren;T. Saito;M. Sakata;T. Sasaki;Z. Shi;M. Shibata;A. Shiomi;T. Shirai;H. Sugimoto;K. Taira;Y. Tan;N. Tateyama;S. Torii;T. Utsugi;C. Wang;H. Wang;X. W. Xu;Y. Yamamoto;G. Yu;A. Yuan;T. Yuda;C. S. Zhang;H. Zhang;J. Zhang;N. Zhang;X. Zhang;Zhaxisangzhu;Zhaxiciren;W. Zhou
在羊八井（海拔4300 m）进行的西藏实验是能量最低的空气簇射阵列，1996年建造的新的高密度阵列对能量低至3 TeV的γ射线空气簇射敏感。使用这个新的阵列，蟹状星云在多TeV的γ射线中被观察到，并在5.5 σ水平上检测到信号。我们还获得了3 TeV以上能区的γ射线能谱，这与成像大气切伦科夫望远镜观测到的γ射线能谱部分重叠。在该能区观测到的Crab谱可用幂律拟合dJ（E）/dE =（4.61 ± 0.90）× 10-12（E/3 TeV）-2.62 0. 17 cm-2 s-1 TeV-1表示。这是第一次用闪烁探测器观测到点源的γ射线信号。
The Tibet experiment, operating at Yangbajing (4300 m above sea level), is the lowest energy air shower array, and the new high-density array constructed in 1996 is sensitive to γ-ray air showers at energies as low as 3 TeV. With this new array, the Crab Nebula was observed in multi-TeV γ-rays and a signal was detected at the 5.5 σ level. We also obtained the energy spectrum of γ-rays in the energy region above 3 TeV which partially overlaps those observed with imaging atmospheric Cerenkov telescopes. The Crab spectrum observed in this energy region can be represented by the power-law fit dJ(E)/dE = (4.61 ± 0.90) × 10-12(E/3 TeV)-2.62±0.17 cm-2 s-1 TeV-1. This is the first observation of γ-ray signals from point sources with a conventional air shower array using scintillation detectors.