The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images
The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images
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DOI：
10.1093/pasj/61.5.999
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发表时间：
2009-10-25
影响因子：
2.3
通讯作者：
Ebisawa, Ken
中科院分区：
文献类型：
--
作者：
Matsuoka, Masaru;Kawasaki, Kazuyoshi;Ebisawa, Ken
全天x射线图像监测（MAXI）任务是安装在国际空间站日本实验舱暴露设施（JEM-EF或Kibo-EF）上的第一个天文有效载荷。它有两种宽视场的x射线狭缝相机和两种x射线探测器，包括能量范围为2至30keV的气体比例计数器和能量范围为0.5至12keV的x射线ccd。MAXI将比以往任何x射线全天监测有效载荷都更强大，能够监测数百个活动星系核。在最佳观测条件下的真实模拟表明，MAXI将在一次国际空间站轨道（90分钟）期间提供类似于20 mCrab(类似于2-30 keV波段的7 x 10(-10) erg cm（-2) s(-1)）的全天x射线源图像，类似于4.5 mCrab一天，类似于2 mCrab一周。在两年的时间里，MAXI的最终可探测性可以接近0.2 mCrab，这与MAXI视场的源混淆极限相当。MAXI的目标是：(1)提醒社区注意x射线新星和瞬态x射线源，(2)监测x射线源的长期变化，(3)激发对可变物体的多波长观测，(4)创建无偏x射线源目录，(5)观测漫射宇宙x射线发射，特别是对低至0.5 keV的软x射线具有更好的能量分辨率。
The Monitor of All-sky X-ray Image (MAXI) mission is the first astronomical payload to be installed on the Japanese Experiment Module - Exposed Facility (JEM-EF or Kibo-EF) on the International Space Station. It has two types of X-ray slit cameras with wide FOVs and two kinds of X-ray detectors consisting of gas proportional counters covering the energy range of 2 to 30keV and X-ray CCDs covering the energy range of 0.5 to 12keV. MAXI will be more powerful than any previous X-ray All Sky Monitor payloads, being able to monitor hundreds of Active Galactic Nuclei. A realistic simulation under optimal observation conditions suggests that MAXI will provide all-sky images of X-ray sources of similar to 20 mCrab (similar to 7 x 10(-10) erg cm(-2) s(-1) in the energy band of 2-30 keV) from observations during one ISS orbit (90 min), similar to 4.5 mCrab for one day, and similar to 2 mCrab for one week. The final detectability of MAXI could be similar to 0.2 mCrab for two years, which is comparable to the source confusion limit of the MAXI field of view (FOV). The MAXI objectives are: (1) to alert the community to X-ray novae and transient X-ray sources, (2) to monitor long-term variabilities of X-ray sources, (3) to stimulate multi-wavelength observations of variable objects, (4) to create unbiased X-ray source cataloges, and (5) to observe diffuse cosmic X-ray emissions, especially with better energy resolution for soft X-rays down to 0.5 keV.