Titlebook: Handbook of X-ray and Gamma-ray Astrophysics; Cosimo Bambi,Andrea Santangelo Living reference work 20220th edition High Energy Astrophysi

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Collimators for X-Ray Astronomical Optics,otect the mirror from severe in-orbit thermal environment or to limit the mirror’s field of view. Although the latter may be a disadvantage in the viewpoint of observational performance, the collimation of incident X-rays allows us to block X-rays with large off-axis angles. Thus, the mount of the X

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Technologies for Advanced X-Ray Mirror Fabrication,or to enable accurate and efficient X-ray reflection. The performance of an X-ray mirror, and ultimately that of the telescope, is linked to the processes and technologies used to create it. The goal of this chapter is to provide the reader with an overview of the different technologies and processe

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Facilities for X-ray Optics Calibration,d. This calibration requires a specialized facility that can approximate an astronomical point source and accommodate the mirrors and other telescope components, including an appropriate detector system. The X-ray source and telescope are typically housed in a vacuum chamber to permit easy propagati

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X-Ray Detectors for Astrophysics,from focusing mirrors characterized by their effective area and angular resolution to a simple collimated system where photons from a small solid angle on the sky are selected. An overview of these optical systems is given in Section 1 of this handbook (.). In this section, we give an introduction t

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Proportional Counters and Microchannel Plates, workhorse for almost four decades. Although the principle of such a detector seems to be rather simple, over time, it underwent considerable performance improvements, and the lifetime under orbital conditions was extended tremendously. Particularly the invention of position-sensitive proportional c

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Charge Coupled Devices,es, and in the case of the “great observatories” of XMM-Newton and Chandra have been returning science data for over 20 years. The CCD optimized for X-ray detection is often different from its variant working in the visible light region. This chapter describes the key performance parameters of relev

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