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长春光学精密机械与物... [3]
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会议论文 [3]
发表日期
2009 [3]
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发表日期:2009
专题:长春光学精密机械与物理研究所
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Blind channel estimation of MIMO-OFDM based on FDPM (EI CONFERENCE)
会议论文
5th International Conference on Wireless Communications, Networking and Mobile Computing, WiCOM 2009, September 24, 2009 - September 26, 2009, Beijing, China
Gang W.
;
Ming Z.
;
Hua C.
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浏览/下载:14/0
  |  
提交时间:2013/03/25
Subspace based methods have been widely discussed in multichannel estimation including MIMO-OFDM system. However
direct subspace methods suffer from heavy computation complexity y of O(N3). In this paper
a new subspace tracking technique called Fast Data Projection Method (FDPM) is proposed for adaptively tracking the noise subspace. The new algorithm has low complexity of O(NL) and is the only numerically stable
low complexity algorithm for tracking subspaces corresponding to the smallest singular values. Simulation results show that the proposed scheme has similar performance to the original. 2009 IEEE.
Detection of low contrast targets based on lifting scheme wavelet transform (EI CONFERENCE)
会议论文
2009 IEEE International Conference on Mechatronics and Automation, ICMA 2009, August 9, 2009 - August 12, 2009, Changchun, China
Chen X.
;
Wang Y.
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浏览/下载:13/0
  |  
提交时间:2013/03/25
This paper present a fast algorithm for detection of low contrast objects by using wavelet filters based on lifting scheme. The advantage is robust to noise. According Swelden's
lifting wavelet filters are biorthogonal wavelet filters containing free parameters. We use reference image of targets to train the lifting terms
so that the learnt wavelet filters have the features of targets. Then applying such filters to the images including targets taken from camera system. We can detect the locations where the high frequency components are almost the same as those of the target image. 2009 IEEE.
The calibration of faint simulation star magnitude based on single photon count technique (EI CONFERENCE)
会议论文
International Symposium on Photoelectronic Detection and Imaging 2009: Advances in Imaging Detectors and Applications, June 17, 2009 - June 19, 2009, Beijing, China
Gan X.-J.
;
Guo J.
;
Xu S.-Y.
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浏览/下载:21/0
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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.
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