Energy sensitivity of the GRAPES-3 EAS array for primary cosmic ray protons
B. Hariharan, S. Ahmad, M. Chakraborty, A. Chandra, S. R. Dugad, S. K. Gupta, Y. Hayashi, H. Kojima, S. S. R. Inbanathan, P. Jagadeesan, A. Jain, P. Jain, V. B.… 展开作者
B. Hariharan, S. Ahmad, M. Chakraborty, A. Chandra, S. R. Dugad, S. K. Gupta, Y. Hayashi, H. Kojima, S. S. R. Inbanathan, P. Jagadeesan, A. Jain, P. Jain, V. B. Jhansi, S. Kawakami, P. K. Mohanty, S. D. Morris, P. K. Nayak, A. Oshima, D. Pattanaik, P. S. Rakshe, K. Ramesh, B. S. Rao, L. V. Reddy, S. Shibata, F. Varsi, M. Zuberi
低能地基宇宙线空气簇射实验的能量阈值一般在几十到几百TeV之间。簇射观测量是用探测器阵列间接测量的。大气对低能二次谐波的吸收限制了它们在地球表面的探测频率。然而，由于选择效应，在低层大气中产生的一小部分低能簇射可以达到观测水平。但由于观测资料较少，重建过程十分困难。因此，人们相信，在低能量下，通过卫星和气球飞行上的实验进行的直接测量更可靠。尽管在低能量下具有非常小的效率（$\sim$ 0.1%），GRAPES-3实验的大接受度（$\sim$ 5 m $^2$ sr）允许观测低于$\sim$ 1 TeV的初级宇宙射线，并开辟了测量从几TeV到超越宇宙射线膝（高达10 $^{16}$ eV）的初级能谱的可能性，覆盖五个数量级。用蒙特卡罗模拟计算了GRAPES-3的初级质子能阈，与实验数据符合较好。此外，还计算了质子原色的总效率和接受度。GRAPES-3实验覆盖如此广泛的能量范围的能力可以提供一个独特的手柄，以桥接低能量下的直接测量和超高能量下的间接测量之间的能谱。
英文摘要：
Low energy ground-based cosmic ray air shower experiments generally have energy threshold in the range of a few tens to a few hundreds of TeV. The shower observables are measured indirectly with an array of detectors. The atmospheric absorption of low energy secondaries limits their detection frequencies at the Earth's surface. However, due to selection effects, a tiny fraction of low energy showers, which are produced in the lower atmosphere can reach the observational level. But, due to less information of shower observables, the reconstruction of these showers are arduous. Hence, it is believed that direct measurements by experiments aboard on satellites and balloon flights are more reliable at low energies. Despite having very small efficiency ($\sim$0.1%) at low energies, the large acceptance ($\sim$5 m$^2$sr) of GRAPES-3 experiment allows observing primary cosmic rays down below to $\sim$1 TeV and opens up the possibility to measure primary energy spectrum spanning from a few TeV to beyond cosmic ray knee (up to 10$^{16}$ eV), covering five orders of magnitude. The GRAPES-3 energy threshold for primary protons through Monte Carlo simulations are calculated, which gives reasonably good agreement with data. Furthermore, the total efficiencies and acceptance are also calculated for protons primaries. The ability of GRAPES-3 experiment to cover such a broader energy range may provide a unique handle to bridge the energy spectrum between direct measurements at low energies and indirect measurements at ultra-high energies.
Demonstrating of Cosmic Ray Characteristics by Estimating the Cherenkov Light Lateral Distribution Function for Yakutsk Array as a Function of the Zenith Angle
State Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories, CAS（中国科学院国家天文台射电天文与技术重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）
Analysis of the TAIGA-HiSCORE Data Using the Latent Space of Autoencoders
Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics（罗蒙诺索夫莫斯科国立大学，斯科贝利辛核物理研究所）；Institute for Informatics and Automation Problems of the National Academy of Science of the Republic of Armenia（亚美尼亚国家科学院信息与自动化问题研究所）；Research Institute of Applied Physics（应用物理研究 institutes）
A simulation study on few parameters of Cherenkov photons in extensive air showers of different primaries incident at various zenith angles over a high altitude observation level
