极化干涉SAR森林树高提取算法的对比分析

在对极化干涉SAR森林树高反演的DEM差值算法、相干相位-幅度综合反演算法进行分析的基础上,对基于极化干涉相干优化方法的改进算法进行了探讨。利用黑龙江大兴安岭地区的一对ALOS全极化干涉SAR数据进行实验,并对比分析各算法的反演结果。结果表明,在使用改进的算法进行森林树高反演时可以获取精度较高的反演结果,并且在一定程度上提高了森林树高反演的稳定性,为森林树高反演工作的业务化运行提供一定的依据。     

正交实验法在测绘中的应用

以检测数字水准仪及标尺综合精度为例，介绍了正交实验法在测绘领域中的应用。     

正交实验法在测绘仪器检定中的应用

在测绘生产和科研项目中，为了改革旧工艺或对新仪器，新产品,经常需要做多因素实验，如何安排多因素实验，是一个很值得研究的问题，文中以数字水准仪及标尺综合精度的检定为例，介绍了正交实验法在测绘仪器检定中的应用。     

河外射电源的结合阵数据的图像处理

不同类型的射电望远镜阵的分辨率差异甚大，用它们的数据进行图像处理后所得到的源结构的尺度也不一样。为了得到中间尺度的结构信息，有时我们需要把不同类型的射电望远镜阵的观测数据结合起来再进行图像处理。本文阐述我们把不同类型阵的数据结合时所用的方法；也给出我们使用的方法所获得的结果的实际例子。     

数字水准仪与精密光学水准仪测量精度比较

数字水准仪的出现解决了大地测量仪器中水准仪自动读数与记录问题,对当代测量技术产生了积极的影响.文中介绍了如何采用双频激光干涉仪配合45°平面镜检测数字水准仪的方法,对精密光学水准仪和数字水准仪进行综合精度的评定和比较,并对结果进行了分析.     

数字水准仪与精密光学水准仪测量精度比较

数字水准仪的出现解决了大地测量仪器中水准仪自动读数与记录问题,对当代测量技术产生了积极的影响。文中介绍了如何采用双频激光干涉仪配合45°平面镜检测数字水准仪的方法,对精密光学水准仪和数字水准仪进行综合精度的评定和比较,并对结果进行了分析。     

Luciola hypertelescope space observatory: versatile, upgradable high-resolution imaging, from stars to deep-field cosmology

Luciola is a large (1 km) “multi-aperture densified-pupil imaging interferometer”, or “hypertelescope” employing many small apertures, rather than a few large ones, for obtaining direct snapshot images with a high information content. A diluted collector mirror, deployed in space as a flotilla of small mirrors, focuses a sky image which is exploited by several beam-combiner spaceships. Each contains a “pupil densifier” micro-lens array to avoid the diffractive spread and image attenuation caused by the small sub-apertures. The elucidation of hypertelescope imaging properties during the last decade has shown that many small apertures tend to be far more efficient, regarding the science yield, than a few large ones providing a comparable collecting area. For similar underlying physical reasons, radio-astronomy has also evolved in the direction of many-antenna systems such as the proposed Low Frequency Array having “hundreds of thousands of individual receivers”. With its high limiting magnitude, reaching the m _v?=?30 limit of HST when 100 collectors of 25 cm will match its collecting area, high-resolution direct imaging in multiple channels, broad spectral coverage from the 1,200 Å ultra-violet to the 20 μm infra-red, apodization, coronagraphic and spectroscopic capabilities, the proposed hypertelescope observatory addresses very broad and innovative science covering different areas of ESA’s Cosmic Vision program. In the initial phase, a focal spacecraft covering the UV to near IR spectral range of EMCCD photon-counting cameras (currently 200 to 1,000 nm), will image details on the surface of many stars, as well as their environment, including multiple stars and clusters. Spectra will be obtained for each resel. It will also image neutron star, black-hole and micro-quasar candidates, as well as active galactic nuclei, quasars, gravitational lenses, and other Cosmic Vision targets observable with the initial modest crowding limit. With subsequent upgrade missions, the spectral coverage can be extended from 120 nm to 20 μm, using four detectors carried by two to four focal spacecraft. The number of collector mirrors in the flotilla can also be increased from 12 to 100 and possibly 1,000. The imaging and spectroscopy of habitable exoplanets in the mid infra-red then becomes feasible once the collecting area reaches 6 m², using a specialized mid infra-red focal spacecraft. Calculations (Boccaletti et al., Icarus 145, 628–636, 2000) have shown that hypertelescope coronagraphy has unequalled sensitivity for detecting, at mid infra-red wavelengths, faint exoplanets within the exo-zodiacal glare. Later upgrades will enable the more difficult imaging and spectroscopy of these faint objects at visible wavelengths, using refined techniques of adaptive coronagraphy (Labeyrie and Le Coroller 2004). Together, the infra-red and visible spectral data carry rich information on the possible presence of life. The close environment of the central black-hole in the Milky Way will be imageable with unprecedented detail in the near infra-red. Cosmological imaging of remote galaxies at the limit of the known universe is also expected, from the ultra-violet to the near infra-red, following the first upgrade, and with greatly increasing sensitivity through successive upgrades. These areas will indeed greatly benefit from the upgrades, in terms of dynamic range, limiting complexity of the objects to be imaged, size of the elementary “Direct Imaging Field”, and limiting magnitude, approaching that of an 8-m space telescope when 1,000 apertures of 25 cm are installed. Similar gains will occur for addressing fundamental problems in physics and cosmology, particularly when observing neutron stars and black holes, single or binary, including the giant black holes, with accretion disks and jets, in active galactic nuclei beyond the Milky Way. Gravitational lensing and micro-lensing patterns, including time-variable patterns and perhaps millisecond lensing flashes which may be beamed by diffraction from sub-stellar masses at sub-parsec distances (Labeyrie, Astron Astrophys 284, 689, 1994), will also be observable initially in the favourable cases, and upgrades will greatly improve the number of observable objects. The observability of gravitational waves emitted by binary lensing masses, in the form of modulated lensing patterns, is a debated issue (Ragazzoni et al., MNRAS 345, 100–110, 2003) but will also become addressable observationally. The technology readiness of Luciola approaches levels where low-orbit testing and stepwise implementation will become feasible in the 2015–2025 time frame. For the following decades beyond 2020, once accurate formation flying techniques will be mastered, much larger hypertelescopes such as the proposed 100 km Exo-Earth Imager and the 100,000 km Neutron Star Imager should also become feasible. Luciola is therefore also seen as a precursor toward such very powerful instruments.     

基于GRACE-FO的微波与激光星间测距数据的重力场模型对比分析

为分析GRACE-FO微波测距系统KBR及激光干涉测距系统LRI对时变重力场结果的影响,以动力学方法为基础,分别采用KBR数据和LRI数据反演2019-01~2021-08的90阶无约束时变重力场模型APM_KBR和APM_LRI,并进行对比分析。 从重力场模型阶方差和等效水柱高的空间分布来看,在两类测距数据完整且质量较好的前提下,两者精度处于同一水平,而当发生较多月卫星机动或其他卫星事件时会使LRI数据缺失,从而导致APM_LRI模型在该月得到的等效水柱高时间序列信噪比略低。由后验残差结果可知,APM_LRI后验残差RMS比APM_KBR减少约50%,且在高频处(大于等于60 CPR)LRI的后验残差显著低于KBR。总体来说,在现有条件下,由于背景场模型等其他因素影响,两类测距数据反演重力场的阶方差和等效水柱高结果基本一致,但后验残差上LRI测距具有更低的噪声。因此,未来可直接使用LRI测距数据探测、分析较弱的地球物理信号。     

大动态宽带干涉式雷电测向接收机新技术

提出了一种基于非线性盲辨识的自适应数字接收机技术。由于宽带雷电信号的时频特征未知或时变,在频域对宽带数字接收机输出信号中的谐波与互调分量进行识别和分选,并以其短时能量最小化作为其非线性行为模型参数的盲辨识准则,利用最速下降算法实现模型参数的自适应提取和更新,然后在线实时地对接收机输出信号进行非线性补偿。实验结果表明,该盲辨识数字接收技术可以将整机的无杂散失真动态范围（SFDR）提高近20dB,极有利于在强干扰存在时对微弱信号的接收与检测。     

用于断层测量的温度补偿光纤外腔型法布里-珀罗位移传感器

针对光纤EFPI传感器通常尺寸很小,而断层尺寸相对较大,导致光纤EFPI传感器在待测断层处安装不便的情况,提出了一种可用于断层测量的光纤外腔型法布里-珀罗位移传感器.两根陶瓷插芯从陶瓷套管的两端插入构成EFPI结构,通过使用金属内管和金属外管,增大了光纤EFPI位移传感器的尺寸;并且金属外管的两端采用O型圈密封,因此该EFPI位移传感器能够防水防尘.为了消除温度对EFPI位移传感器的影响,两根金属内管采用了不同热膨胀系数的材料在结构上进行温度补偿.在温度连续变化的环境下,对腔长为718.39 m的EFPI位移传感器进行了测量.测量结果显示,经过温度补偿设计后,位移传感器的温度系数由0.14 μm/℃下降到了-0.04 μm/℃,并呈现过补偿.