天文学聚焦x射线光学

P. Gorenstein
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引用次数: 28

摘要

聚焦x射线望远镜是x射线天文学上升到与光学和射电天文学平起平坐的最重要因素。它们是研究高温区的热辐射、磁场中高能粒子的非热同步辐射和低能量光子在x射线波段的逆康普顿散射的主要工具。基于Wolter 1几何结构的聚焦掠射x射线望远镜的四个任务目前正在0.2至10 keV波段的太空中运行。自1999年以来,两个具有成像能力和高分辨率色散光谱仪的天文台级任务一直在运行。它们是美国宇航局的钱德拉x射线天文台,角分辨率为0.5角秒,面积为0.1平方米;欧洲航天局的xmm -牛顿天文台,有3个共对准的望远镜,总有效面积为0.43平方米,分辨率为15角秒。另外两个是日本的Suzaku,它具有较低的空间分辨率和非色散光谱,以及Swift的XRT,它观察并精确定位伽玛射线爆发的x射线余辉。新的任务包括使用更宽带宽的聚焦望远镜和执行新巡天任务的望远镜。美国宇航局、欧空局和日本航天局正在合作开发一个具有非常大有效面积的天文台,用于非常高的能量分辨率色散和非色散光谱。需要新的技术来提高钱德拉望远镜的角度分辨率。自适应光学应该提供适度的改进。然而,数量级的改进只能通过使用物理光学来实现。透射式衍射折射透镜理论上能够实现亚毫角秒分辨率。x射线干涉测量理论上可以达到0.1微弧秒的分辨率,这足以成像附近活动星系中心超大质量黑洞的视界。然而,物理光学系统的焦距在103 ~ 104 km之间,在光学与探测器之间的远程编队飞行精确定位技术发展之前无法实现。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Focusing X-Ray Optics for Astronomy
Focusing X-ray telescopes have been the most important factor in X-ray astronomy’s ascent to equality with optical and radio astronomy. They are the prime tool for studying thermal emission from very high temperature regions, non-thermal synchrotron radiation from very high energy particles in magnetic fields and inverse Compton scattering of lower energy photons into the X-ray band. Four missions with focusing grazing incidence X-ray telescopes based upon the Wolter 1 geometry are currently operating in space within the 0.2 to 10 keV band. Two observatory class missions have been operating since 1999 with both imaging capability and high resolution dispersive spectrometers. They are NASA’s Chandra X-ray Observatory, which has an angular resolution of 0.5 arc seconds and an area of 0.1 m2 and ESA’s XMM-Newton which has 3 co-aligned telescopes with a combined effective area of 0.43 m2 and a resolution of 15 arc seconds. The two others are Japan’s Suzaku with lower spatial resolution and non-dispersive spectroscopy and the XRT of Swift which observes and precisely positions the X-ray afterglows of gamma-ray bursts. New missions include focusing telescopes with much broader bandwidth and telescopes that will perform a new sky survey. NASA, ESA, and Japan’s space agency are collaborating in developing an observatory with very large effective area for very high energy resolution dispersive and non-dispersive spectroscopy. New technologies are required to improve upon the angular resolution of Chandra. Adaptive optics should provide modest improvement. However, orders of magnitude improvement can be achieved only by employing physical optics. Transmitting diffractive-refractive lenses are capable theoretically of achieving sub-milli arc second resolution. X-ray interferometry could in theory achieve 0.1 micro arc second resolution, which is sufficient to image the event horizon of super massive black holes at the center of nearby active galaxies. However, the physical optics systems have focal lengths in the range 103 to 104 km and cannot be realized until the technology for accurately positioned long distance formation flying between optics and detector is developed.
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