Energy determination of gamma-ray induced air showers observed by an extensive air shower array
Energy determination of gamma-ray induced air showers observed by an extensive air shower array
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DOI：
10.1007/s10686-017-9530-9
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发表时间：
2017-03
影响因子：
3
通讯作者：
K. Kawata;T. Sako;M. Ohnishi;M. Takita;Y. Nakamura;K. Munakata
中科院分区：
文献类型：
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作者：
K. Kawata;T. Sako;M. Ohnishi;M. Takita;Y. Nakamura;K. Munakata
我们提出了一个新的能量估计，以确定能量的伽马射线诱导的空气簇射的基础上广泛的空气簇射的能量范围在10 TeV和1000 TeV之间的横向分布。我们进行了详细的Monte Carlo模拟，假设西藏空气簇射阵列位于海拔4,300米的高度。我们定义S50，这表示在50米的空气簇射轴的粒子密度，作为一个新的能量估计。利用S50，在天顶角θ< 20 °的范围内，在100 TeV处的能量分辨率估计为约16%。我们发现，S50给出了一个更好的能量分辨率比27%的空气簇射大小（Ne）和30%的检测粒子的总和（），这已经使用到目前为止，在100 TeV。我们还比较了γ射线和强子宇宙线诱导的空气簇射的年龄分布。年龄参数可能有助于区分初级伽马射线和强子宇宙射线。
We propose a new energy estimator to determine the energies of gamma-ray induced air showers based on the lateral distribution of extensive air showers in the energy range between 10 TeV and 1000 TeV. We carry out a detailed Monte Carlo simulation assuming the Tibet air shower array located at an altitude of 4,300 m above sea level. We define S50, which denotes the particle density at 50 m from the air shower axis, as a new energy estimator. Using S50, the energy resolution is estimated to be approximately 16 % at 100 TeV in the range of the zenith angle𝜃< 20∘. We find S50 giving a better energy resolution than 27 % for the air shower size (Ne) and 30 % for the sum of detected particles (), which have been used so far, at 100 TeV. We also compare the reconstructed age distributions of gamma-ray induced air showers and hadronic cosmic-ray induced air showers. The age parameter may help to discriminate between primary gamma rays and hadronic cosmic rays.