论文标题
用于伽马射线天体物理学的康普顿望远镜
Compton Telescopes for Gamma-ray Astrophysics
论文作者
论文摘要
康普顿望远镜依赖于MEV伽马射线能量范围的主要相互作用机制：康普顿散射。通过精确记录在检测器体积中多个康普顿散射相互作用的位置和能量，可以回收光子的原始方向和能量。这些强大的调查工具可以具有广泛的视野，良好的光谱和两极分化功能，并且可以解决MEV范围内的许多开放科学问题，尤其是来自多中间机天体物理学。第一个基于太空的康普顿望远镜于1991年推出，该领域的进展随着检测器技术的进步而继续。本章将概述康普顿散射的物理和康普顿望远镜操作的基本原理；将讨论电子跟踪和极化功能。简要介绍了康普顿事件重建和成像重建。描述了康普顿望远镜和标准性能参数的点扩散函数，并引入了显着的仪器设计。
Compton telescopes rely on the dominant interaction mechanism in the MeV gamma-ray energy range: Compton scattering. By precisely recording the position and energy of multiple Compton scatter interactions in a detector volume, a photon's original direction and energy can be recovered. These powerful survey instruments can have wide fields of view, good spectroscopy, and polarization capabilities, and can address many of the open science questions in the MeV range, and in particular, from multimessenger astrophysics. The first space-based Compton telescope was launched in 1991 and progress in the field continues with advancements in detector technology. This chapter will give an overview of the physics of Compton scattering and the basic principles of operation of Compton telescopes; electron tracking and polarization capabilities will be discussed. A brief introduction to Compton event reconstruction and imaging reconstruction is given. The point spread function for Compton telescopes and standard performance parameters are described, and notable instrument designs are introduced.
