Simbol-X：在0.5-80 Kev能量段具有前所未有的成像能力的编队飞行任务
Simbol-X: A Formation Flight Mission with an Unprecedented Imaging Capability in the 0.5-80 Kev Energy Band
摘要：
20世纪60年代发现的宇宙源X射线辐射为我们打开了一扇新的强大的宇宙观测窗口。事实上，在70 - 90年代对X射线天空的探索已经将X射线天文学确立为天体物理学的一个基本领域。今天，来自天体物理源的辐射通常以能量低于10 keV而闻名。这种情况的主要原因是纯粹的技术，因为掠入射反射到目前为止仅限于软X射线波段。在10 keV以上，所有的观测都是用准直探测器或编码掩模仪器获得的。为了使10 keV以上的X射线天文学向前迈出一大步，有必要将聚焦X射线光学原理扩展到更高的能量，高达80 keV或更高。为此，意大利航天局和法国空研中心目前正在研究实施一项称为Simbol-X的X射线飞行任务。利用反射镜制造和航天器编队飞行中的新兴技术，Simbol-X将把掠入射成像推向80 keV及以上，与迄今为止在10 keV以上运行的所有仪器相比，在灵敏度和角分辨率方面都有很大的改进。这一技术突破将为天体物理学和宇宙学打开一扇新的高能窗口。在这里，我们将解决这样一个分布式和可变形的仪器的发展的问题。我们将重点介绍望远镜的主要性能，如角分辨率，灵敏度和源定位。我们还将描述分布在两颗卫星上的有效载荷的校准方面的特殊性，因此处于非“冻结”配置。
英文摘要：
The discovery of X-ray emission from cosmic sources in the 1960s has opened a new powerful observing window on the Universe. In fact, the exploration of the X-ray sky during the 70s-90s has established X-ray astronomy as a fundamental field of astrophysics. Today, the emission from astrophysical sources is by large best known at energies below 10 keV. The main reason for this situation is purely technical since grazing incidence reflection has so far been limited to the soft X-ray band. Above 10 keV all the observations have been obtained with collimated detectors or coded mask instruments. To make a leap step forward in X-ray astronomy above 10 keV it is necessary to extend the principle of focusing X ray optics to higher energies, up to 80 keV and beyond. To this end, ASI and CNES are presently studying the implementation of a X-ray mission called Simbol-X. Taking advantage of emerging technology in mirror manufacturing and spacecraft formation flying, Simbol-X will push grazing incidence imaging up to 80 keV and beyond, providing a strong improvement both in sensitivity and angular resolution compared to all instruments that have operated so far above 10 keV. This technological breakthrough will open a new high-energy window in astrophysics and cosmology. Here we will address the problematic of the development for such a distributed and deformable instrument. We will focus on the main performances of the telescope, like angular resolution, sensitivity and source localization. We will also describe the specificity of the calibration aspects of the payload distributed over two satellites and therefore in a not "frozen" configuration.
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