Based on optical diffraction theory and geometry optical, such as diameter of diffraction spot, Point Spread Function (PSF), Strehl Ratio, Modulation Transfer Function (MTF), etc., were analyzed using theoretical analytical expression and numerical simulation of segmented telescope in the paper. The effect of sub-segmented mirrors’ Piston error and Tip-tilt error on far-field was calculated. The results show that both Piston error and tip-tilt error affect system’s Strehl Ratio and MTF and blurred far field image. Tip-title error can cause the generation of piston error. The compensation for the Piston error would highly improve the far field imaging characteristics.

To solve the problem of the vignetting resolution in mosaic CCD camera imaging based on reflector, the multi-radiance vignetting correction algorithm is studied. Firstly, the main reasons of the typically Reflector-based mosaics camera’s vignetting phenomenon were analyzed. Then, analyzing the vignetting images under multi-radiance levels in radiometric calibration experiment, each pixel’s DN (Digital Number) in vignetting imaging region is increasing with the rise of the incident radiance, nearly linear relationship. Finally, the each pixel’s correction factors in vignetting imaging region were calculated using the multi-radiance vignetting correction algorithm, and the correction factors were used to correct vignetting image. In correcting experiments, the original vignetting images’ non-uniformity is above 10%, and corrected images’ non-uniformity is reduced to below 0.5%. Correcting results meet the requirments of non-uniformity of the reflector-baesd mosaics camera.

Abstract: The polarization state of the object is altered due to the surfaces of the optical lens in the polarization CCD camera with large viewing field, and the variation relate to the field of view, azimuth angle and polarization states of the observed beams. The polarimetric accuracies limit the application of polarization remote sensing due to the polarization phenomenon of the instrument. To overcome the problems, calibration method of the model parameters and retrieval of the polarization information is introduced based on the polarimetric calibration model. In order to verify the calibration method feasibility, the Degree of Linear Polarization (DOLP) comparison tests of the calibrated polarization CCD camera with large viewing field compared with the high-precision variable polarization light source have been carried out. Experimental results show that the DOLP accuracy of the calibrated polarization CCD camera is better than 1.18% at the 0°, 15° and 25° field of view. The method of polarimetric calibration would get rid of the influence of polarization phenomena of the polarization CCD camera, and contribute to fundamental basis for the quantitative application of polarization remote sensing information for the Chinese polarized satellite sensor.

Accurate calibration of system parameters is a very important mission in the development of high-accuracy measurement equipment. As for multi-channel shipboard star sensor, calibration of the optical system parameters and the equipment structure parameters is an important prerequisite for accurate positioning. Comprehensively considering origin error, directing error, non-orthogonal of the axes, scale error and inclination error of the optical system, the calibration model and method of the optical system parameters is established. The calibration method of the equipment structure parameters is established according to the structure features of multi-channel. The accuracy of the calibration method is about five arcseconds, which is high enough for positioning accuracy of shipboard star sensor.

For the use of mirrors in space camera back support, the change in temperature will cause a partial supporting surface accuracy of the hole near the lower annular formation of local defects, which affect the quality of the optical system corresponding to the imaging field of view. In order to improve the adaptability to temperature mirror support structure by increasing the flexibility, and reduce the local connection stiffness, design of a flexible structure is optimized. Mirror assembly simulation for analysis, in the mirror assembly temperature 4℃ lower case, optimize the structure of the reflector around the middle hole of the support as the local scene shaped PV=4.9 nm, RMS=1.0 nm. Compared with the former (PV=16.6 nm, RMS=3.5 nm), and its accuracy is improved by 3 times, the global field shape PV=16.3 nm, RMS=3.2 nm. Compared to before optimization (PV=30.2 nm, RMS=5.2 nm), its accuracy is improved. Mirror assembly in the 1 order frequency before the optimization is 191 Hz and after the optimization are 183 Hz, basically unchanged. Mirrors in various gravity conditions, depending on the global scene shaped to optimize PV and RMS values before and after the basic structure remains unchanged, which illustrate that the new flexible support structure ensures the mirror dynamic, static stiffness, improve the temperature adaptability of mirror, reduce the influence of temperature changes to the mirror support hole near the local surface shape accuracy, and improve the imaging quality of local field optical system and imaging quality of all field goal.

To provide higher measure precision of the star sensor attitude, the principles of error that appears because the three Euler angles are influenced by proper motion are studied in this paper. The proper motion level is divided into Ⅰto Ⅸ and stored in the guide star catalogue and the yearly variation of different star proper promotion in the last 20 years according to the output of three Euler angles is analyzed in depth. The simulation experiment results show that the precision can increase over 75″after adjusting the three Euler angles in the last 20 years by QUEST method. The new condition number can be minimized by choosing the star with relatively lower proper motion level to perform the calculation of the attitude when the magnitude of the stars is similar. This can improve the precision and stabilization of the star sensor attitude measurement greatly in the engineering.

Establishing accurate light geometry model, feature and image between the positive and negative calculate formula is derived, which is the key steps of space TDI CCD (charge-coupled device) time delay integral camera dynamic imaging simulation. Stereo mapping satellite link simulation based on ray tracing all the main line, with high precision high resolution surface physical model for the input source, considering the atmospheric radiation transmission, optical system imaging spectral response, detectors and camera noise and so on each link, complete the imaging process end-to-end complete analysis. In visible light optical remote sensing camera, for example, considering the precession of orbit, the earth under the inertial system of precession and nutation TDI CCD stitching, under the condition of complete double array camera ray tracing dynamic imaging geometry modeling, and the model error sources are analyzed. Verified by experiment and analysis, physical model to face the camera geometry precision of 124 m, forward-looking camera positioning accuracy of 193 m, double line array camera is high precision, which satisfies the requirement of the geometrical model of three-dimensional mapping all link simulation.

Phycoerythrin (PE) is an important indicator which measures the algae eutrophication in water. Visible absorption spectrometry has some advantages, such as rapid detection, accurate, no secondary pollution, on-line and in-situ measurements etc. Therefore, the method of detection phycoerythrin contents by visible absorption spectrometry is proposed. Based on the standard solution of phycoerythrin as experimental subjects, the visible absorption spectrometry of the standard solution are collected in the range of 5 ~ 250 mg/L, and the correction analysis model is made. The spectral preprocessing is performed in different spectral region and the Partial Least Squares (PLS) algorithm is used to establish the correction analysis model. Compared with Principal Component Regression (PCR) algorithm, the results show that the correction analysis model has the highest correlation and smallest error by the PLS algorithm made in the spectral region of 480~570 nm. The correlation coefficient root mean square error of calibration and relative standard deviation is 0.9930, 5.5783 and 3.92%, respectively.

Because of the poor efficiency and effectiveness of current visual tracking algorithms, a real-time object tracking algorithm is proposed based on subspace learning. Under the framework of particle filtering, this paper uses the incremental PCA subspace method to learn an orthogonal subspace, and then get the linear representation of target appearance. In order to avoid the tracking drift produced by complicated interference, such as occlusions, motion blur and so on, an observation model and a template update scheme are built, which consider the complicated interference especially occlusions, to solve the drift problem of the traditional observation model based on minimum mean square error. The experimental results show that the algorithm in complicated conditions can be well implemented compared with several state-of-the-art algorithms.

In order to solve the measuring velocity problem on the ground object by the Unmanned Aerial Vehicle (UAV), a measuring velocity method based on visible light is proposed. And the target orientation model is given. The principle of velocity measure is introduced in detail. The algorithm can solve the object velocity through a succession of UAV images.Practical measuring results prove that the velocity error of the algorithm can meet the demands of the ground moving object velocity measuring accuracy.

An algorithm based on SIFT and compressive features is proposed to develop effective and efficient appearance models for robust object tracking due to factors such as pose variation, illumination change, occlusion, and motion blur. The algorithm describes the target and background with compressive features which labeled as positive and negative specimens sampling from frames. The tracking task is formulated as a binary classification via a SVM classifier with online update in the compressed domain. In new frame, utilize the classifier to obtain the target’s position. Meanwhile, introduce SIFT to solve the target size change, so as to achieve adaptive template size. The proposed tracking algorithm performs favorably against state-of-the-art algorithms on challenging sequences in terms of efficiency, accuracy and robustness.

Due to low absorption and negligible non-birefringent character in atmosphere, optical free space therefore serves as the most promising channel for large-scale quantum communication by use of satellites and optical ground stations. Quantum communication in space has become a new technological challenge in the evolving field of quantum communications. Its main goal is to achieve the distribution of single photons or entangled photon pairs from satellites to implement both quantum technologies such as quantum cryptography and fundamental quantum physics experiments. This article describes the equipment and features of the 1.2 m astronomical telescope which will perform experiments with quantum experiment satellite of China. The optical ground station uses 1.2 m gimbaled telescope to collect the photons, and the strategy of the system is slightly developed to meet the need of tracking LEO satellite, which has coarse and fine loop, and it can also control a transmitting and receiving laser beam within a few micro radians jitter. This telescope with multiple functions will play an important role in space-to-ground quantum communication.

Receiver plane is an important component of Visible Light Communication (VLC) system, and its receiving angle will affect the performance of system. In traditional VLC system, a vertical optical receiver plane is used, receivers may locate at some places far away from LED source, where the Signal to Noise Ratio (SNR) is much smaller than other areas. At the same time, the peak-to-valley value of SNR is so large. In this paper, we propose and design tilting receiver plane based on Genetic Algorithm to reduce the peak-to-valley value of SNR, and improve the uniform distribution of SNR in a whole room. Based on the numerical results of the proposed indoor VLC system, when using the tilting receiver, the SNR distribution will be improved in VLC system in the use of tilting receiver. The results of numerical analysis show that in the case of one LED source, there is a 4.98 dB improvement of peak-to-valley SNR value. In the case of four LED sources, there is a 2.51 dB improvement of peak-to-valley value of SNR. Hence, the tilting receiver can be proposed to improve the performance of VLC system.

One of the most important factors for influencing interferometer measurement accuracy is coherent noise recently. To improve measurement accuracy, the coherent noise of interferometric system should be reduced effectively. Ring light source as an effective means to suppress the coherent noise has been widely used in engineering practice. In this paper, with different ring radius, the interference measurement accuracy is analyzed based on interferometer model. And the influence of interference measurement results increase in a certain ring radius, along with the increase of interference cavity length. Simulation results show that, with the increase of the ring light source ring radius, the system error of measurement results increase with the increase of the ring radius, in the same ring radius, with cavity length be longer, the system error of measurement is greater.

An algorithm of correction of random phase-shifts error is proposed by applying Lissajous calibration technology to PSI. Proposed method does not have to calculate the true phase shifts of each interferogram, which directly estimate the phase extraction error (typically a non linear combination of offset, bias, less of quadrature) of PSA first and then correct them. Simulation results show that proposed method can effectively correct the phase extraction error from a series of (>3) interferograms with random phase-shifts errors without any iterations. The algorithm is fast, accurate and adapt to all kinds of PSAs. Experimental results indicate that proposed method has a comparative precision with AIA but is far faster than AIA.