New hybrid reconstruction techniques for first analyses of ultra-high energy gamma-ray data from the hybrid TAIGA detector

最高能量的银河宇宙射线的加速器，pevatron，还没有被确定。在超高能量伽玛射线区（ebbb10 TeV到几个100 TeV）进行灵敏的伽玛射线观测对这项任务至关重要。为了覆盖这个能量范围，需要一个非常大的仪器面积（几平方公里）。目前现有的和计划中的仪器采用了成熟的方法，即立体成像空气切伦科夫望远镜（例如，HESS， MAGIC， VERITAS， CTA）或非成像粒子阵雨前采样阵列（HAWC， LHAASO）。德国和俄罗斯的TAIGA实验开创了一种混合方法，它将大间距切伦科夫望远镜与切伦科夫光定时阵列结合在一起。在一种新的混合重建方法中，将单个望远镜图像与时序阵列的时序和振幅信息相结合。在我们的初步工作中，我们已经证明这种组合达到了与经典立体阵列相当的性能，同时大大减少了所需的望远镜数量。该提案的主要目标是开发和验证新的和优化的混合成像/定时重建技术，使用广泛和现实的空气淋室和探测器模拟。我们将这些方法应用于初始TAIGA数据，并对突出目标进行首次敏感点源分析。随着调试数据的采集，我们将探索蟹状星云发射光谱的超高能量端，观察工作中的电子peatron。最后，我们将在这个新的观测窗口中开发超高能量伽马射线观测的物理案例（粒子加速，光子传播，重暗物质等）。

The accelerators of the highest energy Galactic cosmic rays, the Pevatrons, are yet to be identified. Sensitive gamma-ray observations in the ultra-high energy gamma-ray regime (E>10 TeV up to several 100 TeV) are essential for this task. In order to cover this energy range, a very large instrumented area (several square kilometers) is required. The currently existing and planned instruments follow the well-established approaches of either stereoscopic imaging air Cherenkov telescopes (e.g., HESS, MAGIC, VERITAS, CTA) or non-imaging particle shower-front sampling arrays (HAWC, LHAASO). The German-Russian TAIGA experiment is pioneering a hybrid approach, which combines widely spaced Cherenkov telescopes with a Cherenkov light timing array. The individual telescope images are combined with the timing and amplitude information from the timing array in a novel hybrid reconstruction method. In our preliminary work, we have shown that such a combination reaches a performance comparable to classical stereoscopic arrays, while dramatically reducing the required number of telescopes.The main objective of this proposal is the development and verification of new and optimized hybrid imaging/timing reconstruction techniques, using extensive and realistic air shower and detector simulations. We will apply these methods to initial TAIGA data and carry out the first sensitive point source analyses of prominent objects. With the commissioning data to be taken, we will explore the ultra-high energy end of the Crab nebula emission spectrum, observing an electron Pevatron at work. Finally, we will develop the physics case (particle acceleration, photon propagation, heavy dark matter etc.) for ultra-high energy gamma-ray observations in this new observational window.