The intrinsic spectra of some distant blazars known as “extreme TeV blazars” have shown a hint at an anomalous hardening in the TeV energy region. Several extragalactic propagation models have been proposed to explain this possible excess transparency of the Universe to gamma-rays starting from a model which assumes the existence of so-called axion-like particles (ALPs) and the new process of gamma-ALP oscillations. Alternative models suppose that some of the observable gamma-rays are produced in the intergalactic cascades. This work focuses on investigating the spectral and angular features of one of the cascade models, the Intergalactic Hadronic Cascade Model (IHCM) in the contemporary astrophysical models of Extragalactic Magnetic Field (EGMF). For IHCM, EGMF largely determines the deflection of primary cosmic rays and electrons of intergalactic cascades and, thus, is of vital importance. Contemporary Hackstein models are considered in this paper and compared to the model of Dolag. The models assumed are based on simulations of the local part of large-scale structure of the Universe and differ in the assumptions for the seed field. This work provides spectral energy distributions (SEDs) and angular extensions of two extreme TeV blazars, 1ES 0229+200 and 1ES 0414+009. It is demonstrated that observable SEDs inside a typical point spread function of imaging atmospheric Cherenkov telescopes (IACTs) for IHCM would exhibit a characteristic high-energy attenuation compared to the ones obtained in hadronic models that do not consider EGMF, which makes it possible to distinguish among these models. At the same time, the spectra for IHCM models would have longer high energy tails than some available spectra for the ALP models and the universal spectra for the Electromagnetic Cascade Model (ECM). The analysis of the IHCM observable angular extensions shows that the sources would likely be identified by most IACTs not as point sources but rather as extended ones. These spectra could later be compared with future observation data of such instruments as Cherenkov Telescope Array (CTA) and LHAASO.

中文翻译：

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在当代天体物理 EGMF 模型中对来自星系际质子引发的级联的极端 TeV 耀变体的伽马射线 SED 和角扩展进行建模

一些被称为“极端 TeV 耀变体”的遥远耀变体的本征光谱暗示了 TeV 能量区域的异常硬化。已经提出了几个河外传播模型来解释宇宙对伽马射线的这种可能的过度透明，该模型从假设存在所谓的轴子状粒子 (ALP) 和伽马-ALP 振荡的新过程的模型开始。替代模型假设一些可观测的伽马射线是在星系际级联中产生的。这项工作的重点是研究当代银河外磁场 (EGMF) 天体物理模型中的一个级联模型——星系间强子级联模型 (IHCM) 的光谱和角度特征。对于 IHCM，EGMF 在很大程度上决定了初级宇宙射线和星系间级联电子的偏转，因此至关重要。本文考虑了当代 Hackstein 模型，并与 Dolag 模型进行了比较。假设的模型基于对宇宙大尺度结构局部部分的模拟，并且在种子场的假设上有所不同。这项工作提供了两个极端 TeV 耀变体 1ES 0229+200 和 1ES 0414+009 的光谱能量分布 (SED) 和角扩展。结果表明，与在不考虑 EGMF 的强子模型中获得的相比，IHCM 成像大气切伦科夫望远镜 (IACT) 的典型点扩散函数内的可观测 SED 将表现出特征性的高能量衰减，这使得区分在这些模型中。同时，与 ALP 模型的某些可用光谱和电磁级联模型 (ECM) 的通用光谱相比，IHCM 模型的光谱具有更长的高能尾。对 IHCM 可观察角扩展的分析表明，大多数 IACT 可能不会将这些源识别为点源，而是将其识别为扩展源。这些光谱稍后可以与切伦科夫望远镜阵列 (CTA) 和 LHAASO 等仪器的未来观测数据进行比较。对 IHCM 可观察角扩展的分析表明，大多数 IACT 可能不会将这些源识别为点源，而是将其识别为扩展源。这些光谱稍后可以与切伦科夫望远镜阵列 (CTA) 和 LHAASO 等仪器的未来观测数据进行比较。对 IHCM 可观测角度扩展的分析表明，大多数 IACT 可能不会将源识别为点源，而是将其识别为扩展源。这些光谱稍后可以与切伦科夫望远镜阵列 (CTA) 和 LHAASO 等仪器的未来观测数据进行比较。