Astronomical object imaging system

Abstract

The invention provides an astronomical object imaging system. According to the technical scheme of the invention, the system comprises a telescope objective lens, a wide-spectrum polarization splitting prism, a central control device, a digital miniature reflector type spatial light modulator, a first camera, a second camera, a first relay lens, a second relay lens, a third relay lens, a fourth relay lens, and a wide-spectrum quarter-wave plate. The first relay lens is located between the telescope objective lens and the wide-spectrum polarization splitting prism. The second relay lens is located between the wide-spectrum polarization splitting prism and the second camera. The third relay lens is located between the wide-spectrum polarization splitting prism and the digital miniature reflector type spatial light modulator. The fourth relay lens is located between the wide-spectrum polarization splitting prism and the first camera. The wide-spectrum quarter-wave plate is located between the wide-spectrum polarization splitting prism and the third relay lens. The first, second, third and fourth relay lens are respectively opposite to four usable surfaces of the wide-spectrum polarization splitting prism for placement. The system can achieve the clear imaging of a big-view-field astronomical object.

Description

technical field [0001] The invention belongs to the technical field of astronomical target imaging, relates to a method and system for clear imaging of astronomical targets, and further relates to a method and system for realizing clear imaging of astronomical targets by evaluating the defocused image quality of point targets. Background technique [0002] At present, there are three main methods for imaging astronomical targets, namely adaptive optics method, image deconvolution method and lucky imaging method. Adaptive optics methods are expensive and only work with small fields of view. Image deconvolution methods are time-consuming and have limited improvement in image quality. The method of lucky imaging obtains clear imaging of astronomical targets by taking long-time shots of the target, selecting those with excellent imaging from the image sequence and superimposing them. This method is simple to implement and low in cost, and has been widely used. [0003] In orde...

AI Technical Summary

Problems solved by technology

However, the image quality is related to the intensity of atmospheric turbulence. The index of energy concentration of a point target cannot accurately describe the intensity of atmospheric turbulence, so it is not suitable for evaluating image quality.

The gray gradient evaluation method evaluates the imaging quality by calculating the contrast of the target contour in the image. When this method is applied to an extended astronomical target, because the image contains many halo regions, the imaging quality of each halo region changes independently, which will lead to The probability of the entire clear image appearing is very low, so that the selected image has serious blurring problems in local areas

[0004] The mechanism of atmospheric turbulence is complex, and the light field emitted by the target will be randomly disturbed

Traditional imaging methods obtain imaging results by superimposing target disturbance light fields. This process does not use atmospheric disturbance information, and the real light field distribution cannot be reconstructed from the image.

Therefore, without using guide stars to assist imaging, it is difficult to judge directly from the target image whether its imaging is disturbed by the atmosphere, or the degree of interference

Images