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	Catadioptric optical system design of 15-magnitude star sensor with large entrance pupil diameter 期刊论文 OAI收割 Sensors (Switzerland), 2020, 卷号: 20, 期号: 19, 页码: 1-14 作者: Bai, Yang; Li, Jianlin; Zha, Rongwei; Wang, Ying; Lei, Guangzhi \| 收藏 \| 浏览/下载：42/0 \| 提交时间：2020/11/02 star sensor catadioptric optical system COS large entrance pupil diameter di use spot 15-magnitude
	Detection ability analysis of ground based imaging polarization detector 期刊论文 OAI收割 optik, 2015, 卷号: 126, 期号: 23, 页码: 4771-4774 作者: Yao, Dalei; Wen, Desheng; Xue, Jianru; Qiu, Yuehong; Xi, Jiangbo 收藏 \| 浏览/下载：25/0 \| 提交时间：2015/12/25 Polarization detection Degree of polarization Signal-to-noise ratio Detection ability Star magnitude
	Relating basic properties of bright early-type dwarf galaxies to their location in Abell 901/902 期刊论文 OAI收割 ASTRONOMY & ASTROPHYSICS , 2009, 卷号: 508, 期号: 2, 页码: 665-675 Barazza F. D.; Wolf C.; Gray M. E.; Zheng, X 收藏 \| 浏览/下载：13/0 \| 提交时间：2011/12/08 DIGITAL SKY SURVEY COLOR-MAGNITUDE RELATION STAR-FORMATION HISTORIES VIRGO-CLUSTER SURVEY ELLIPTIC GALAXIES SPACE-TELESCOPE COMA CLUSTER SPIRAL GALAXIES STELLAR POPULATIONS SPHEROIDAL GALAXIES
	The calibration of faint simulation star magnitude based on single photon count technique (EI CONFERENCE) 会议论文 OAI收割 International Symposium on Photoelectronic Detection and Imaging 2009: Advances in Imaging Detectors and Applications, June 17, 2009 - June 19, 2009, Beijing, China 作者: Xu S.-Y.; Guo J.; Guo J. 收藏 \| 浏览/下载：32/0 \| 提交时间：2013/03/25 A calibration method of faint star magnitude of the star scene simulation device is proposed in this paper. In the research of simulation star magnitude luminometers and CCD devices are the general calibration devices which are used to measure the illumination intensity and calibrate its magnitude. But if the simulation magnitude is only sixth magnitude its illumination intensity is only 1.010-8 Lux. This illumination intensity level is the lowest illumination intensity that the commercial luminometer can detect. Hence the simulation star magnitude lower than six magnitude cannot be calibrated by luminoters. Likewise CCD devices also need an additive cooler in this case. When the single photon characteristic is presented due to the low luminosity of simulating light sources the simulation star magnitude can be calibrated by detecting its photon flux of radiation with the method of single photon count. In this paper the detection principle of single photon based on a compact designed PMT detecting of the radiation level of simulation star magnitude is advanced. Especially a spectrum match method is proved theoretically to be an effective means for selecting PMT photosensitive type. In the case of the detection object of the simulation star in visible wavelength a analysis indicates that the material of tri-alkali cathode materials its best choice after being compared the Signal-to-Noise of photon detector of several PMT photosensitive materials based on the different spectrum match ratio of different object light sources and different cathode materials. An experiment is employed to show the relationship of control voltage of PMT and its dark counter the relationship of the environment temperature of PMT and its dark counter which proves its only decades of CPS at room temperature. The so low dark counter avoids a bulky cooler and is convenient for installing it on the star scene simulation equipment. Finally in the experiment of calibrating the simulation star magnitudes the ability of its calibration is confirmed to reaches up to 12m meanwhile its calibration error is within 0.2m. 2009 SPIE.
	Design of a scene simulator in land-based aerospace lab with the man-made light source system based on quantum theory (EI CONFERENCE) 会议论文 OAI收割 Optoelectronic Devices and Integration II, November 12, 2007 - November 15, 2007, Beijing, China 作者: Fang W.; Yi W. 收藏 \| 浏览/下载：29/0 \| 提交时间：2013/03/25 The paper presents a method with the technique of combination filtering of spectrum and the technique of DSP control for the simulation and recognition of the spontaneously lightening object and stellar map in the universe. The magnitude and the spectrum of a star can be simulated in a wide dynamic range. We established the mathematical models of the Vega's visible light spectrum and luminous flux density. Tungsten-halogen lamp as a light source is used to fit the linear light of the spontaneously lightening object in the universe. Through the experiment it shows that the more sub-channels there are while filtering spectrum in the visible spectrum and the more degrees the variable neutral density filters and the narrow-band attenuators have more close to the actual spectrum the simulated spectrum is. It is proved that using the PID technique is beneficial to the output of the accurate and steady radiation from the light sources. The experiment shows that the using of this method can get perfect result in fitting and simulating the spectrum magnitude and the stellar map of the spontaneously lightening object . The analysis of the consistent result and the experimental error is also discussed in detail in this paper.
	Study on the detection sensitivity of APS star tracker (EI CONFERENCE) 会议论文 OAI收割 3rd International Symposium on Advanced Optical Manufacturing and Testing Technologies: Optical Test and Measurement Technology and Equipment, July 8, 2007 - July 12, 2007, Chengdu, China 作者: Li J.; Li J.; Li J.; Liu J.; Liu J. 收藏 \| 浏览/下载：23/0 \| 提交时间：2013/03/25 Detection sensitivity is an important parameter of star tracker which can express detection limit of the weakest detected visual star magnitude. Detection sensitivity of APS star tracker is related to APS parameters optical system aperture and lens permeance rate SNR and so on. This paper the expressions of APS star detected signal and APS noise are given so signal-noise ratio (SNR) of star tracker can be obtained. And based on the theory inspecting signal from noise and optimal SNR threshold detection principle the detection sensitivity model can be obtained. The corresponding APS star tracker detection limit is obtain based on APS IBIS5 and general optical system parameter design. When SNR threshold is 8.1 which can obtain 99.9% detection probability we can calculate that the detection sensitivity is 6.5 visual magnitude.