共查询到20条相似文献,搜索用时 156 毫秒
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本文给出类星体3C286在λ18厘米的MERLIN图像、VLBI图像和MERLIN+VLBI图像.呈现在MERLIN图像上的低亮度的结构在MERLIN VLBI联合阵的图像上基本被分解,仅留下一些支离破碎的痕迹.MERLIN+VLBI图像的中央部分比VLBI图像有更长的延伸.MERLIN+VLBI图像的动态范围好于1000:1,但没有搜索到反向喷流.我们提出了几种可能的模式对所得到的结构进行解释. 相似文献
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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
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利用WinView软件进行图像处理 总被引:1,自引:1,他引:0
WinView是一个用于图像采集和处理的软件包。在图像处理方法,具有很强的图像后处理功能,它除了能对图像进行线性、非线性、像素合并、多图关联和阈值处理外,还能对图像进行边增强、锐化、平滑等处理。本文详细介绍了这些功能及在天文观测上的应用,以期对使用这个软件的观测者有所帮助。 相似文献
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《天文研究与技术》2016,(1)
在射电综合成像领域,通常需要用退卷积的方法补全频域稀疏的采样。由于扩展源的频域信息更为丰富,要补全这些信息相对于点源来说更难,因此扩展源的图像重建是射电综合成像领域的一大难点。为了探索射电干涉扩展源图像重建方法的特点,将最大熵与一种加速的CLEAN方法(文中称之为Multi-Point CLEAN,MP-CLEAN)对扩展源的干涉阵模拟数据的图像重建进行了比较。通过比较,发现对于同样的观测数据,两种方法都能较好地重建图像,但MP-CLEAN方法的旁瓣祛除效果与重建效果优于最大熵方法,而且在模拟数据重建中MP-CLEAN方法的总体速度比最大熵快3倍以上。最后,在讨论部分通过研究两种方法中参数的选择对重建结果的影响,发现最大熵方法比MP-CLEAN方法对参数选择的依赖性弱,这表明最大熵方法有更好的鲁棒性。 相似文献
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地基望远镜在成像过程中,由于受大气湍流、望远镜静态像差、跟踪误差、指向误差及视场变化的影响,不同视场区域的PSF (Point Spread Function)具有差异;同时,不同望远镜获取的图像PSF也存在差异.将多个望远镜获取的星象直接叠加至相同的区域后,图像质量受像质最差的望远镜限制,最终观测分辨率和灵敏度均会受到影响.通过图像复原,可以提高图像质量,进而提高叠加效果.根据该思路提出了1种基于PSF分区的迭代图像复原方法:该方法首先通过SOM (Self-organizing Maps)对PSF进行聚类分析,利用同类别PSF的平均PSF进行反卷积,再将反卷积结果按PSF聚类结果分割为不同大小的子图,最后将子图进行拼接.图像复原在提高图像质量的同时,降低了PSF不一致性对图像叠加带来的影响.将几个望远镜在同一时刻获取的图像经反卷积处理之后利用图像配准算法进行矫正并叠加,可获得高信噪比图像.对实际望远镜获取的数据处理后的结果表明:图像在进行复原和叠加过程中,星象目标信噪比不断提升,提高了成像系统对暗星的探测能力. 相似文献
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OSIPOV S. N. GANDZHA S. I. ANDRIYENKO O. V. KARPOV M. V. KOSTIK R. I. 《Solar physics》1997,172(1-2):361-370
The primary shortcomings of existing methods for spectrophotometry of the Sun as a star are discussed. A new observational method is proposed. This method is based on a repeated scanning of the Sun's image while summing the signal of each step across the solar disk. A device for precise spectrophotometry of the Sun as a star has been developed around a double-pass spectrograph. This device and its operation algorithm are described. Errors caused by scanning irregularities and seeing are estimated. Several Sun-as-a-star spectrum line profiles and their bisectors are presented and compared with the same ones from the Kitt Peak FTS solar flux atlas. 相似文献
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斑点干涉成像技术是克服大气湍流影响,提高地面大口径望远镜分辨本领的有效途径之一。该技术利用斑点相机拍摄一系列的短曝光像,使得大气湍流冻结,再经过图像处理获得高分辨率重建像。该技术设备简单,易于实现,很快在观测天文学中得到了广泛的应用,尤其是对双星的研究。首先回顾了天文高分辨率重建技术的发展,并介绍了相关研究成果。描述了几种典型的斑点干涉成像处理方法及其优缺点。对图像噪声类型及滤波方法进行了分析。在上海天文台1.56m望远镜上开展了双星斑点干涉观测实验,目标星等4~7mag,双星目标星等差小于2。分别采用斑点干涉术和迭代位移叠加法成功实现了双星目标的高分辨率成像,初步证明了在1.56m望远镜上进行斑点干涉成像实验,能够达到接近望远镜衍射极限的分辨率水平。 相似文献
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A principle of restoration methods based on multichannel blind deconvolution (MBD) is introduced. The methods assume that
for every un-degraded unobservable image several degraded observed images are available. It is better conditioned than classical
single channel approach. The first algorithm represents a generalization of iterative deconvolution scheme introduced for
single images. The second MBD algorithm is based on so-called subspace technique. The subspace method is not iterative and
this possibly implies an implementation that can be computationally more efficient. Both methods are presented in applications
to artificial image data (computer-generated multichannel degraded data) with known ideal image to get a comparison with restored
one. Performance in a real situation on solar photosphere images is shown. 相似文献
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F. P. Pijpers 《Monthly notices of the Royal Astronomical Society》1999,307(3):659-668
An unbiased method for improving the resolution of astronomical images is presented. The strategy at the core of this method is to establish a linear transformation between the recorded image and an improved image at some desirable resolution. In order to establish this transformation only the actual point spread function and a desired point spread function need be known. No image actually recorded is used in establishing the linear transformation between the recorded and improved image.
This method has a number of advantages over other methods currently in use. It is not iterative, which means it is not necessary to impose any criteria, objective or otherwise, to stop the iterations. The method does not require an artificial separation of the image into 'smooth' and 'point-like' components, and thus is unbiased with respect to the character of structures present in the image. The method produces a linear transformation between the recorded image and the deconvolved image, and therefore the propagation of pixel-by-pixel flux error estimates into the deconvolved image is trivial. It is explicitly constrained to preserve photometry and should be robust against random errors. 相似文献
This method has a number of advantages over other methods currently in use. It is not iterative, which means it is not necessary to impose any criteria, objective or otherwise, to stop the iterations. The method does not require an artificial separation of the image into 'smooth' and 'point-like' components, and thus is unbiased with respect to the character of structures present in the image. The method produces a linear transformation between the recorded image and the deconvolved image, and therefore the propagation of pixel-by-pixel flux error estimates into the deconvolved image is trivial. It is explicitly constrained to preserve photometry and should be robust against random errors. 相似文献
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500 m口径球面射电望远镜(Five-hundred-meter Aperture Spherical Radio Telescope,FAST)是一个超大口径的可动望远镜,有三项技术创新,一是选址,二是轻型馈源索支撑,三是主动反射面。在主动反射面上,单元面板的面型和面板的出厂加工精度对电磁波在反射面的汇聚有很大影响。FAST主反射面由4 600块三角形反射面板拼接而成,每块面板为边长11 m三角形,这对FAST反射面面板的测量技术提出了更高的要求。摄影测量直接在影像上进行量测,无需接触物体本身;所摄影像信息丰富,可以从中获得所研究物体的大量几何信息和物理信息;适用于大范围、多目标测量,效率高。目前世界上最大的射电望远镜,如GBT和ARECIBO都是采用摄影测量技术进行反射面面形检测。在对现有的面型检测技术调研并试验后,提出基于数字近景摄影测量的方法,对FAST反射面11 m单元面板的面型进行检测,数分钟完成反射面板面型的一次检测,测量精度达到2.5 mm,经过调整后的单元面板的面型精度达到了3.0 mm,结果表明摄影测量应用于FAST反射面单元面板面型检测是可行的。 相似文献
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首先介绍了斑点图形成机制以及获取方法,并借助计算机模拟了斑点图的生成。然后重点描述斑点图的图像重建方法,包括频率域和空间域重建方法。在频率域重建方法部分依次详细叙述了用于复原模信息的斑点干涉法和用于复原相位信息的由模复原相位法、Knox-Thompson法、斑点掩模法;空间域重建方法部分介绍了典型的LWH法和迭代位移叠加法;另外,盲消卷积法也为斑点图重建提供了新的思路,文章对此方法也做了介绍;特别地,还对国内在该领域的相关工作做了介绍;关于斑点图重建方法在天文学、天体物理学等领域的应用,文章做了有针对性的介绍;最后一章是斑点图图像重建方法的总结。 相似文献
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In this investigation, a comparison is made of two methods for developing perturbation theories for non-canonical dynamical systems. The methods compared are the generalized Lie-Hori method and the method of averaging. In the comparison presented here, the equivalence of the methods up to the second order in the small parameter is shown. However, the approach used can be extended to demonstrate the equivalence for higher orders. To illustrate the equivalence Duffing's equation, the van der Pol equation and the oscillator with quadratic damping problem are solved using each method. 相似文献
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When using γ-ray coded-mask cameras, one does not get a direct image as in classical optical cameras but the correlation of the mask response with the source. Therefore the data must be mathematically treated in order to reconstruct the original sky sources. Generally this reconstruction is based on linear methods, such as correlating the detector plane with a reconstruction array, or non-linear ones such as iterative or maximization methods (i.e. the EM algorithm). The latter have a better performance but they increase the computational complexity by taking a lot of time to reconstruct an image. Here we present a method for speeding up such kind of algorithms by making use of a neural network with a back-propagation learning rule. 相似文献