During astronomical observations, the CCD sensor will produce the smear effect during frame transfer, and the smear effect will pollute the column pixels corresponding to the image, thus affecting target detection. According to the characteristics of frame transfer CCD, the generation of smear effect is analyzed, and the gray scale analysis model of the smear effect is established, which simulates the gray value corresponding to the smear effect generated by astronomical observation cameras when detecting targets of different magnitudes and verifies it through experiments. The theoretical analysis in this paper provides an important reference for the design of astronomical cameras.
KEYWORDS: Interference (communication), Charge-coupled devices, Denoising, Electrons, Cadmium sulfide, Analog to digital converters, Analog electronics, Tunable filters, Signal processing, Linear filtering
As a new low noise CCD signal processing technology, digital correlation double sampling noise reduction technology is widely used in the field of faint astronomical target detection. In this paper, various noise sources of CCD video processing circuit are studied, the characteristics of various noises are analyzed deeply, the mathematical model of CCD circuit noise is established, and a noise reduction method based on digital correlation double sampling technology is proposed. Through simulation modeling of CCD noise signal, the simulation results show that the digital correlation double sampling method using double Gaussian filter function has a good effect on noise suppression.
In view of the background interference of the current multi-point laser target source positioning detection system, positioning accuracy and real-time performance need to be improved. Based on the DM6437 hardware platform, an embedded multi-point laser target positioning system is designed. The collection of image information is completed by CMOS camera and TVP5158 chip. The DM6437 chip realizes tasks such as algorithm processing and data transmission. Experimental results show that the target location algorithm based on threshold and shape effectively removes the interfering light source in the image background. Therefore, the accuracy of laser target location is greatly improved. The positioning system based on the DSP hardware platform is small in size, stable in operation, and has high application promotion value.
In order to break through the bottleneck of traditional CCD camera in suppressing noise, this paper designs a new system of digital domain correlation double sampling. The CCD video signal is digitized by a high-speed, high-resolution A/D converter at a sampling frequency much higher than the readout rate, and then an optimal digital signal processing algorithm is designed for the characteristics of the CCD signal readout noise to suppress noise. Experiments show that the system can suppress the readout noise at 8.1 e- at 500K read rate, which can reduce the output noise of CCD more effectively.
For a positioning CMOS camera, we put forward a system which can measure quantitatively dispersed spot parameters and the degree of energy concentration of certain optical system. Based on this method, the detection capability of the positioning CMOS camera can be verified. The measuring method contains some key instruments, such as 550mm collimator, 0.2mm star point, turntable and a positioning CMOS camera. Firstly, the definition of dispersed spot parameters is introduced. Then, the steps of measuring dispersed spot parameters are listed. The energy center of dispersed spot is calculated using centroid algorithm, and then a bivariate-error least squares curve Gaussian fitting method is presented to fit dispersion spot energy distribution curve. Finally, the connected region shaped by the energy contour of the defocused spots is analyzed. The diameter equal to the area which is 80% of the total energy of defocused spots and the energy percentage to the 3×3 central area of the image size are both calculated. The experimental results show that 80% of the total energy of defocused spots is concentrated in the diameter of the inner circle of 15μm, and the percentage to the 3×3 pixels central area can achieve 80% and even higher. Therefore, the method meets the needs of the optical systems in positioning CMOS camera for the imaging quality control.
The traditional CCD offset correction processing method is to obtain normal exposure image and dark field image respectively. In the later image processing, use normal exposure image minus the dark field image. Although traditional method can offset correction, but cannot to realize real-time offset correction. Because the traditional method is to obtain offset correction after acquire normal exposure image and dark field image, while the normal exposure image and dark field image is not acquired at the same time. This method would reduce the offset correction precision. A novel method to real-time offset correction for frame transfer CCD is proposed in this paper. The method is based on the improvement of the traditional frame transfer CCD driving timing and CCD signal processing sequence. The traditional frame transfer CCD driving timing is exposure, frame transfer and read CCD level shift register. An offset correction line is added before read CCD data storage area to acquire the offset variation of the each frame image. Take it as a normal image data. In CCD signal processing algorithm to offset calculation and correction. This novel method can correct the offset of each frame image each pixel data real time. In this way the effect on the images from the variation of the offset caused by factors such as the working temperature and the aging of electronic devices in CCD signal processing circuit of CCD camera is restrained.
Detection capability of space camera is regarded as the principal parameter in the design of space camera. On the basis of the concept of signal-to-noise ratio (SNR) and through the research of principles and derivation of theories, detection capabilities under static condition and the condition of relative motion were analyzed and compared. With a set of typical parameters given, the change of detectable magnitude with the changes of parameters was investigated. Considering the real operating environment of space camera, the necessity of temperature control in the design of space camera was discussed. The theoretical analysis provides a reference for the design of space camera.
The article presents a new method to detect small moving targets in space surveillance. Image sequences are processed to detect and track targets under the assumption that the data samples are spatially registered. Maximum value projection and normalization are performed to reduce the data samples and eliminate the background clutter. Targets are then detected through connected component analysis. The velocities of the targets are estimated by centroid localization and least squares regression. The estimated velocities are utilized to track the targets. A sliding neighborhood operation is performed prior to target detection to significantly reduce the computation while preserving as much target information as possible. Actual data samples are acquired to test the proposed method. Experimental results show that the method can efficiently detect small moving targets and track their traces accurately. The centroid locating precision and tracking accuracy of the method are within a pixel.
KEYWORDS: Video processing, Cameras, Charge-coupled devices, Astronomy, CCD cameras, Field programmable gate arrays, Signal to noise ratio, Amplifiers, Data conversion, Video
To satisfy the requirement of the astronomical observation, a novel timing sequence of frame transfer CCD is proposed. The multiple functions such as the adjustments of work pattern, exposure time and frame frequency are achieved. There are four work patterns: normal, standby, zero exposure and test. The adjustment of exposure time can set multiple exposure time according to the astronomical observation. The fame frequency can be adjusted when dark target is imaged and the maximum exposure time cannot satisfy the requirement. On the design of the video processing, offset correction and adjustment of multiple gains are proposed. Offset correction is used for eliminating the fixed pattern noise of CCD. Three gains pattern can improve the signal to noise ratio of astronomical observation. Finally, the images in different situations are collected and the system readout noise is calculated. The calculation results show that the designs in this paper are practicable.
The low noise video process chain design is the important guarantee of realization of CCD detection performance. While pre-amplifier locate in the front end of the video signal process of CCD camera, so the low noise preamplifier design is the important guarantee of realization of low noise CCD camera. Firstly, calculate the bandwidth and equivalent noise bandwidth of video process chain of CCD camera. Secondly, design the preamplifier circuit and build the noise model of the preamplifier. Thirdly, according to the noise model calculation the noise of the pre-amplifier. Lastly, build the noise simulation model of the preamplifier. Through theoretical calculation and PSPICE simulation result predict the noise level of the preamplifier of the CCD .The noise level of the preamplifier less than 2 electronics, it meets specification requirement.
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