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SW-MW Infrared Spectrometer for Lunar Mission

机译:用于月球任务的SW-MW红外光谱仪

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SW-MW Imaging Infrared Spectrometer, the Hyperspectral optical imaging instrument is envisaged to map geomorphology and mineralogy of lunar surface. The instrument is designed to image the electro-magnetic energy emanating from moon's surface with high spectral and spatial resolution for the mission duration from an altitude of 100 km. It is designed to cover 0.8 to 5 μm in 250 spectral bands with GSD 80m and swath 20km. Primarily, there are three basic optical segments in the spectrometer. They are fore optics, dispersing element and focusing elements. The payload is designed around a custom developed multi-blaze convex grating optimized for system throughput. The considerations for optimization are lunar radiation, instrument background, optical throughput, and detector sensitivity. HgCdTe (cooled using a rotary Stirling cooler) based detector array (500×256 elements, 30um) is being custom developed for the spectrometer. Stray light background flux is minimized using a multi-band filter cooled to cryogenic temperature. Mechanical system realization is being performed considering requirements such as structural, opto-mechanical, thermal, and alignment. The entire EOM is planned to be maintained at ~240K to reduce and control instrument background. Al based mirror, grating, and EOM housing is being developed to maintain structural requirements along with optomechanical and thermal. Multi-tier radiative isolation and multi-stage radiative cooling approach is selected for maintaining the EOM temperature. EOM along with precision electronics packages are planned to be placed on the outer and inner side of Anti-sun side (ASS) deck. Power and Cooler drive electronics packages are planned to be placed on bottom side of ASS panel. Cooler drive electronics is being custom developed to maintain the detector temperature within 100mK during the imaging phase. Low noise detector electronics development is critical for maintaining the NETD requirements at different target temperatures. Subsequent segments of the paper bring out system design aspects and trade-off analyses.
机译:SW-MW成像红外光谱仪,即高光谱光学成像仪,用于绘制月球表面的地貌和矿物学图。该仪器旨在以高光谱和空间分辨率对从月球表面发出的电磁能量进行成像,以完成从100 km高度开始的任务持续时间。它的设计覆盖GSD 80m和20km范围的250个光谱带中的0.8至5μm。首先,光谱仪中有三个基本的光学部分。它们是前光学,分散元件和聚焦元件。有效负载围绕为系统吞吐量优化的定制开发的多火焰凸面光栅而设计。优化的考虑因素包括月球辐射,仪器背景,光通量和探测器灵敏度。基于HgCdTe(使用旋转式斯特林冷却器冷却)的探测器阵列(500×256元素,30um)是为光谱仪定制开发的。使用冷却至低温的多波段滤光片可将杂散光的背景通量降至最低。考虑到诸如结构,光机械,热和对准等要求,正在执行机械系统实现。计划将整个EOM维持在〜240K,以减少和控制仪器的背景。正在开发基于铝的反射镜,光栅和EOM外壳,以保持结构要求以及光机和热学性能。选择了多层辐射隔离和多级辐射冷却方法来维持EOM温度。计划将EOM与精密电子封装一起放在防日光(ASS)甲板的外侧和内侧。电源和冷却器驱动器电子组件计划放置在ASS面板的底部。正在定制开发冷却器驱动电子设备,以在成像阶段将探测器温度保持在100mK以内。低噪声检测器电子学的发展对于在不同目标温度下维持NETD要求至关重要。本文的后续部分介绍了系统设计方面和权衡分析。

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