共查询到20条相似文献，搜索用时 31 毫秒
1.
《天文和天体物理学研究(英文版)》2014,(8)
In order to implement an observing strategy,image degradation that occurs during optical observation of space debris is ineluctable and has distinct characteristics. Image restoration is presented as a way to remove the influence of degradation in CCD images of space debris,based on assumed PSF models with the same FWHM as images of the object. In the process of image restoration,the maximum entropy method is adopted. The results of reduction using observed raw CCD images indicate that the precision in estimating positions of objects is improved and the effects of degradation are reduced. Improving the astrometry of space debris using image restoration is effective and feasible. 相似文献
2.
利用计算机数值模拟的方法，对等功率谱滤波方法的图像恢复效果进行测定，原始清晰图像选用以（0，0）为圆心的台阶式灰度图，且台阶灰度值非常接近，这些清晰图像首先进行系统退化，然后加入噪声（本文选用白噪声）生成脏图，图像恢复采用等功率谱滤波器，并将信噪比简化为常数k，图像恢复效果的好坏，用恢复后图像的信噪经和台阶的陡度（台阶的下底宽减上底宽，单位为像素个数）来定量测量，并结合普通图像的恢复，进行定性的视觉观察，主要测量退化图像的信噪比对图像恢复效果的影响，结果是：当信噪比＞15：1，图像恢复效果较好，当信噪比小于该值时，图像恢复效果较差，当信噪比下降到5：1时，图像恢复效果极差，几乎无法辨认，其次是系统传递函H对图像恢复效果的影响，也进行了一些讨论，最后，通过对实际的天文图像进行恢复，验证了测量过程的合理性和结果的正确性，并列举了等功率谱波器的一个典型应用，即在同态滤波器中使用等功率谱滤波器的传递函数。 相似文献
3.
We propose a criterion for extending the parameter search method (Krishnakumar and Venkatakrishnan, 1997) of estimating the point spread function to solar data. In the parameter search method, the number of pixels with negative intensity values in the restored object is used as an estimator for determining the unknown parameters of the point spread function. As a solar image has a high background, the restored object does not contain negative values, thereby making the method unsuitable for solar data. We propose to use the intrinsic contrast of solar features as a criterion for identifying the unknown parameter. We validate our method through simulations. This method can not be used for image restoration but can be used for monitoring daytime seeing. 相似文献
4.
《天文和天体物理学研究(英文版)》2020,(7)
Taking a large number of images, the Cassini Imaging Science Subsystem(ISS) has been routinely used in astrometry. In ISS images, disk-resolved objects often lead to false detection of stars that disturb the camera pointing correction. The aim of this study was to develop an automated processing method to remove the false image stars in disk-resolved objects in ISS images. The method included the following steps:extracting edges, segmenting boundary arcs, fitting circles and excluding false image stars. The proposed method was tested using 200 ISS images. Preliminary experimental results show that it can remove the false image stars in more than 95% of ISS images with disk-resolved objects in a fully automatic manner,i.e., outperforming the traditional circle detection based on Circular Hough Transform(CHT) by 17%. In addition, its speed is more than twice as fast as that of the CHT method. It is also more robust(no manual parameter tuning is needed) when compared with CHT. The proposed method was also applied to a set of ISS images of Rhea to eliminate the mismatch in pointing correction in automatic procedure. Experiment results showed that the precision of final astrometry results can be improve by roughly 2 times that of automatic procedure without the method. It proved that the proposed method is helpful in the astrometry of ISS images in a fully automatic manner. 相似文献
5.
During the 5-year-observational phase of Gaia several one-dimensional observations will be obtained from the same objects at different epochs and transit angles. Combining the information from all the transits to produce a single two-dimensional image is scientifically important as this will allow to detect much fainter stars in the vicinity of the main source than otherwise possible from single observations on-board the satellite or from individual transmitted patches. Most of the emerging objects will be physical companions, but some background/foreground objects will also be found. The combination procedure further increases the image resolution in the across scan-direction. The procedure consists of combining patches that are stretched back to 2-D windows, only possible since the centroid positions of the windows are known. The initial image window from which the patches originate is not square, but elongated along the scan-direction if the Astro AF11 field of view is used in the current calculations. Transit angles can take any value between 0∘ and 360∘. The window combining method is a simple mapping procedure that is fast and should handle all realistic complexities occurring during the Gaia data reduction. The method is not intended to be a perfect image restoration technique, but its purpose is to fulfill the scientific requirement of detecting faint neighboring sources existing in the close vicinity of the main targets. In this study we show examples of the combined windows and illustrate how faint companions around primary targets could be detected. We investigate the performances and limitations of the method and discuss possible complexities that might occur during the final data analysis. 相似文献
6.
Imaging Atmospheric Cherenkov Telescopes (IACTs) need imaging optics with large apertures and high image intensities to map the faint Cherenkov light emitted from cosmic ray air showers onto their image sensors. Segmented reflectors fulfill these needs, and as they are composed from mass production mirror facets they are inexpensive and lightweight. However, as the overall image is a superposition of the individual facet images, alignment is a challenge. Here we present a computer vision based star tracking alignment method, which also works for limited or changing star light visibility. Our method normalizes the mirror facet reflection intensities to become independent of the reference star’s intensity or the cloud coverage. Using two CCD cameras, our method records the mirror facet orientations asynchronously of the telescope drive system, and thus makes the method easy to integrate into existing telescopes. It can be combined with remote facet actuation, but does not require one to work. Furthermore, it can reconstruct all individual mirror facet point spread functions without moving any mirror. We present alignment results on the 4 m First Geiger-mode Avalanche Cherenkov Telescope (FACT). 相似文献
7.
We have implemented a multiscale vision model based on the wavelet transform to analyse field astronomical images. The discrete transform is performed by the à trous algorithm. The vision model is based on the notion of significant structures. We identify the pixels of the associated wavelet transform space (WTS) with the objects. For each scale a region labelling is carried out. An interscale connectivity graph is then established. In accordance with some rules that permit false detections to be removed, the objects and their sub-objects are identified. They define respectively trees and sub-trees in the graph. In this way, the identification of the WTS pixels of the tree related to a given object leads to the reconstruction of its image by the conjugate gradient method. The model has been tested successfully on simulated images of stars and galaxies which allow us to show the capabilities of the detection and restoration procedures of the model. Finally, tests on real images show that one can analyse complex structures better than with classical astronomical vision models. 相似文献
8.
Atmospheric turbulence severely restricts the spatial resolution of astronomical images obtained by a large ground-based telescope. In order to reduce effectively this effect, we propose a method of blind deconvolution, with a bandwidth constraint determined by the parameters of the telescope's optical system based on the principle of maximum likelihood estimation, in which the convolution error function is minimized by using the conjugate gradient algorithm. A relation between the parameters of the telescope optical system and the image's frequency-domain bandwidth is established, and the speed of convergence of the algorithm is improved by using the positivity constraint on the variables and the limited-bandwidth constraint on the point spread function. To avoid the effective Fourier frequencies exceed the cut-off frequency, it is required that each single image element (e.g., the pixel in the CCD imaging) in the sampling focal plane should be smaller than one fourth of the diameter of the diffraction spot. In the algorithm, no object-centered constraint was used, so the proposed method is suitable for the image restoration of a whole field of objects. By the computer simulation and by the restoration of an actually-observed image of α Piscium, the effectiveness of the proposed method is demonstrated. 相似文献
9.
10.
The effectiveness of equal power spectrum filtering in image restoration is analyzed via digital simulation. We start with a gray-scale map of concentric rings with different grey values. To obtain a dirty image, the original image is first transformed via a linear space-invariant system. Then, white noise is mixed into the image. The equal power spectrum filter is then used for the image restoration. The signal to noise ratio (SNR) and a defined steepness of the steps, together with the visual impression, are accepted to characterize the performance of the image restoration. It is concluded that a satisfactory restoration can be realized when the SNR > 15. When SNR < 5, the image is completely un-restorable. The effect of system's transfer function on image restoration is also discussed. The effectiveness of the presented model of equal power spectrum filter is confirmed by applying it to the restoration of an actual astronomical image. Finally, a typical application of the equal power spectrum filter is given. 相似文献
11.
Miura Noriaki Baba Naoshi Sakurai Takashi Ichimoto Kiyoshi Soltau Dirk Brandt Peter 《Solar physics》1999,187(2):347-356
A method for the improvement of resolution in an observed solar image is proposed. A blind deconvolution method is used for
restoration of an atmospherically-degraded solar image, and a super-resolution method is applied to its restored image to
improve the resolution. It is confirmed that a blind deconvolution process can restore fine structures that are blurred in
an observed image, and that the super-resolution process can make a cutoff frequency in a blind-deconvolved image higher.
A time series of super-resolved images of a sunspot observed with the 70-cm Vacuum Tower Telescope at Teide Observatory is
presented. 相似文献
12.
13.
14.
We have obtained deep 6, 20 and 90 cm observation of two of the richest globular clusters in the galaxy, Terzan 5 and Liller
1. In addition to the well known eclipsing pulsar, PSR1744-24A, our 20 cm image of Terzan 5 displays numerous point sources
within 30″, or 4 core radii of the cluster center. The density of these objects rises rapidly toward the core, where an elongated
region of emission is found. This feature may be due to the presence of a higher density of point sources than can be resolved
by the 1″ resolution of our data. Observations at 6 and 90 cm show that the brightest individual sources, as well as the extended
emission, possess the steep spectra expected of pulsars. Furthermore, we find that the strength of the sources in the 20 cm
image agrees well with the standard pulsar luminosity function. The total luminosity and number of objects observed in Terzan
5 suggest that this cluster may contain 100 pulsars — probably more than any other Galactic cluster. Although we do not resolve
individual sources in Liller 1, comparison of our images with other observations suggests that we are again observing the
sum of emission from a number of objects. The 90 cm flux densities of Terzan 5 and Liller 1 are 35 and 9 mJy, respectively,
implying that a number of bright pulsars in these clusters have been hidden from pulsed searches, perhaps by a combination
of dispersion smearing, scattering and doppler broadening. 相似文献
15.
Restricted by the observational condition and the hardware, adaptive optics can only make a partial correction of the optical images blurred by atmospheric turbulence. A postprocessing method based on frame selection and multi-frame blind deconvolution is proposed for the restoration of high-resolution adaptive optics images. By frame selection we mean we first make a selection of the degraded (blurred) images for participation in the iterative blind deconvolution calculation, with no need of any a priori knowledge, and with only a positivity constraint. This method has been applied to the restoration of some stellar images observed by the 61-element adaptive optics system installed on the Yunnan Observatory 1.2m telescope. The experimental results indicate that this method can effectively compensate for the residual errors of the adaptive optics system on the image, and the restored image can reach the diffraction-limited quality. 相似文献
16.
17.
幸运成像技术是一种从大量短曝光图像中选取少量幸运好图进行配准、叠加的高分辨率图像恢复技术,能够有效减小大气湍流对图像质量的影响,但传统的基于中央处理器(Central Processing Unit,CPU)的幸运成像算法难以实现实时化。利用现场可编程门阵列(Field Programmable Gate Array,FPGA)的并行性和灵活性优势,提出了一种新的基于现场可编程门阵列的幸运成像算法,并构建了一个现场可编程门阵列实验系统。该算法采用一种固定选图数且无需排序的图像选择策略和一种以行列坐标为基准的图像配准策略,能够有效节省算法处理时间和硬件资源,达到实时幸运成像的目的。实时幸运成像算法能够以简洁的方式在中小规模的现场可编程门阵列上实现,所得高分辨率图像与基于传统中央处理器算法处理的结果完全相同。实验表明,对于2000帧128×128像素的输入图像进行幸运成像,本算法的运行速度比本实验室之前提出的算法快27倍,比传统的基于CPU+MATLAB幸运成像算法速度快150多倍,处理帧率可达197帧/秒。该算法及其现场可编程门阵列实现技术可以用于构建真正实时的幸运成像系统。 相似文献
18.
大气湍流极大限制了地基大口径望远镜观测天文目标图像的空间分辨率.根据最大似然估计原理,提出了用实际光学带宽约束的可有效减小天文观测图像中大气湍流影响的盲反卷积方法,通过共轭梯度优化算法使卷积误差函数趋向最小.建立了望远镜光学系统参数和图像频域带宽的关系,采用变量正性约束、点扩散函数带宽有限约束,提高算法的收敛性.为避免图像处理中有效傅立叶变换频率超出截止频率,要求采集望远镜焦面图像时单个成像单元(如CCD像素单元)应小于四分之一衍射斑直径.算法中未用目标支持域约束,所提出的方法适用于全视场天文图像恢复.用计算机模拟和对实际天文目标双鱼座图像数据的恢复结果验证了所提出方法的有效性. 相似文献
19.
本文着重指出了在今后处理大面积CCD图象数据过程中,所将面临的数据存贮困难问题.本文提出了一种有效的不丢失天文信息的压缩CCD图象数据的方法,对银纬b=-60°的一个天区的试验表明,压缩后的图象数据仅为原图象数据的1/30左右,并且可以十分方便地进行图象再现及再处理。在压缩数据过程中,我们在剑桥APM底片扫描机参数化施密特照相底片的基础上,重新安排了CCD图象上天体的对应参数,并视天体的大小及形状,有效地提取保存了天体周围矩阵信息. 相似文献
20.
A direct restoration method for spectral and image analysis 总被引：1，自引：0，他引：1
Physical constraints to directly control the output restoration are introduced in each iteration of solving the spectral or image formation equation. For the purpose of increasing the restoration sensitivity and the capability of smoothing noises, the fitting technique is used to reform the resolved equation. Our reconstruction results for Monte Carlo samples and observation data from space high energy astronomy show that, in comparison with traditional restorations, the direct method has high sensitivity, high resolution ability and capability of effectively reducing the effect of statistical fluctuation in data and can be used in the case of poor statistics. This method is model independent and has the capability to simultaneously represent both the extended and discrete features in object. 相似文献