A method of imaging a remote object

 

The invention relates to the field of physical optics and can be used in optical astronomy. Its application allows to obtain a technical result in increased resolution due to the possibility of increasing the size of the multi-element optical system. This technical result is achieved due to the fact that the way pre-recorded distribution of the radiation intensity, which determines the modulus of the correlation function of the field, find a polygonal area in which is inscribed a remote object, choose the intensity distribution of the radiation is equal to zero outside the polygonal region and different from zero inside this area, these data are Fourier image, then build the box in which the distribution phase coincides with the phase distribution of the field Fourier image, and the amplitude distribution coincides with the previously defined by the modulus of the correlation function, then produces the inverse Fourier transform, the process of iteration is repeated to obtain an undistorted image of the remote object. 3 Il.

The present invention relates to the field of technical physics and physical optics, and can be spanou the Earth's atmosphere using a multi-element optical system (MEOS) resolution, corresponding to the size of the aperture of the system.

Known way to find unbiased atmosphere of the phase spectrum in the centers of isolated areas of spatial frequencies generated mnogopotochnoy optical system IAOS (the so-called “method of closed phase” [1]).

The disadvantage of this method is its limited applicability, since it can be used only in IAOS, the diameters of the apertures are substantially smaller than the correlation field for atmospheric distortions (~10 cm [2]). A small area of the apertures of the components of the system, severely limits the amount of light recorded in korotkosostavnom the image of the object, and leads to a low accuracy of the recovery phase and the formation of the image of the object.

Closest to the technical nature of the solution (prototype) of the proposed method is a method [3] obtain images of distant objects in a turbulent atmosphere, based on the distorted image, with the aid of a telescope, in which prior to receiving radiation from the object to measure the value of variancefatmospheric phase distortions limit the spectral range of the light beams of the received radiation valuewhere0- the average wavelength of the received radiation, perform the spectral decomposition of the light beams of the received radiation, scaled by light beams with linearly dependent on the wavelength of the reduction factorand focusing the resulting light beams to create an image object.

One of the main disadvantages of the prototype is the need to apply large (> 10 cm) aperture optical elements, and the quality of these elements should correspond to the diffraction at the aperture. This means, first, the high cost of these optical elements, and secondly, the actual impossibility of manufacturing large quantities to create a very large apertures. Namely, large aperture capable of providing a maximum resolution of objects deleted over long distances. In addition, there are great technical difficulties of combining a large number of light beams received from many telescopes, in one focused beam, in which get the picture.

Using the present invention the technical result consists in the simplification of the method, increasing ratemy and cheaper devices, implement this method.

In accordance with the invention the technical result is achieved by a method for imaging a remote object observed through the turbulent environment, based on the distorted image using mnogoopytnogo telescope, pre-recorded distribution of the radiation intensity, which determines the modulus of the correlation function of the field, then by the limited spatial Fourier image of this module and distorted image of the object in the object plane are polygonal area in which is inscribed the remote object on at least four sides of this area, choose the intensity distribution of the radiation is equal to zero outside the polygonal region and arbitrary, different from zero inside this area, these data are Fourier transform in the plane of the receiving aperture of the telescope as the first iteration, then build the box in which the distribution phase coincides with the phase distribution of the field Fourier image, and the amplitude distribution coincides with the previously defined by the modulus of the correlation function, and then produce an inverse Fourier transform to obtain the field distribution in the subject flat is Aleut beyond its borders, the process of iteration is repeated to obtain an undistorted image of the remote object.

The proposed method can be implemented with the help of the device schematically depicted in Fig.1.

The radiation from the object 1 through the turbulent atmosphere 2 arrives on standard telescope 3, which can only be obtained distorted image of the object, and the photodetector array 4, which registers the intensity distribution of the incident radiation. A distorted image in the telescope 3, and information on the distribution of the radiation intensity from the matrix 4, processed in the correlator field 5 and the Converter Fourier 6, enter the analyzer, image size 7, which is defined by a polygonal area in which the object resides.

Further information from the analyzer 7 and the correlator field 5 enters the block of iterations, which consists of the imaging unit 8, the transducer Fourier 9, the field shaper 10 and transducer Fourier 11, in which after each iteration there is a correction of a distorted image.

After a given number of iterations adjusted image is displayed on the monitor 12.

In Fig.2 shows a main part of a mathematical program, m is Lenogo object,

R - matrix of the polygon which contains the object,

F is the matrix of autocorrelation,

- the associated phase.

In Fig.3 presents the results of one machine experiments, where

and - the original scanned image,

b - distorted image,

with the outline of the original image,

d - restored image.

Mathematically, the modulus of the correlation function field K() is determined from the known relation [4]:

where I(r) - registered intensity, I is the average intensity, and K() is the correlation function of the field defined by the correlator field 5 (Fig.1).

In (1) averaging refers to the integration area for a specific implementation in the case of monochromatic radiation or time-averaging works intensities of the fields at different points in case nemonokhromaticheskogo radiation.

Thus, the task of finding an undistorted image is to find the phase of the correlation function of the field corresponding to the undistorted image, because the module has already been found.

Using the ratio of the van Citter - Zernike [4]:

and- p is the apparent ratio of:

and given the fact that the object has a finite size, we find in the object plane of the rectangle where the function V(x,y), referring to its four sides. Dividing the rectangle into four equal parts by the perpendiculars drawn from the midpoints of its adjacent sides, and selecting one of them, it will be a rectangle, in which the focused object and its boundary points relate to all four sides of the rectangle. Using previously obtained an ordinary telescope distorted image of the object, you can adjust the rectangle to a polygon, inside of which will be the subject (such as a polygon, you can use the profile distorted image), referring to at least four of its sides.

This procedure is performed by the analyzer, image size 7.

Search undistorted image is performed by the following algorithm. For the zero approximation in the imaging unit 8 selects the intensity distribution with zero intensity outside of the received polygon and a non-zero distribution inside (distribution inside can be homogeneous or consider infoe overview recording plane intensity. The field shaper 10, leaving unchanged the phase, as the distribution of the amplitude takes |K() | is the modulus of the correlation function of the field. In the Converter Fourier 11 is the inverse Fourier transform. Next, in the object plane of the imaging unit 8 is left unchanged distribution falling within the polygon, and sinuses nepobedimie. The procedure is repeated again, and so on, because the distribution of intensities corresponding to an exact image of the object is the only naturhouse adjustment as a result of the iterations, the repetition of the above procedure will come to the distribution of intensities corresponding undistorted image of the object.

The company had conducted an experiment on a computer using mathematical package D - 2000” and the graphical editor int Shop-7. At the same time as the subject of the study was selected portrait (Fig.3). Using scanner portrait otsifrovana (256 grayscale) and the digitized information is sent to the computer, which had formed the original object (Fig.3A). This object is distorted using the graphical editor int Shop-7 (Fig.3b). Next on the proposed algorithm, based on the th of the distorted image (Fig.3b), received undistorted image (Fig.3d).

The proposed method can be applied to the creation of wide-aperture systems with angular resolution better than existing telescopic system 1-2 orders of magnitude due to the significant increase in the size of the receiving aperture, with low sensitivity measurements of the correlation function to the turbulence of the atmosphere. The analysis shows the reality of the creation of such telescopes with apertures - 10-1000 m, insensitive to atmospheric distortion.

Sources of information

1. Rhodes W., I. Goodman, 1973, V. 63, N6, p. 647-657.

2. Roddier F. The effects of atmospheric turbulence in optical astronimy, 1981, p. 156.

3. Backout P. A., Milovzorov Centuries, Pakhomov, A. A., Rozhkov A. A., Rahin A. D., He, K. N., RF patent №2062501, priority from 20.06.96 prototype.

4. Born M., Wolf. Principles of optics. - M.: Nauka, 1973.

Claims

A method of imaging a remote object observed through the turbulent environment, based on the distorted image using mnogoopytnogo telescope, wherein the pre-recorded distribution of the radiation intensity, which determines the modulus of the correlation function of the field, then the spatial limited Fu is here, in which is inscribed the remote object on at least four sides of this area, choose the intensity distribution of the radiation is equal to zero outside the polygonal region, and an arbitrary non-zero inside this area, these data are Fourier transform in the plane of the receiving aperture of the telescope as the first iteration, then build the box in which the distribution phase coincides with the phase distribution of the field Fourier image, and the amplitude distribution coincides with the previously defined by the modulus of the correlation function, and then produce an inverse Fourier transform to obtain the field distribution in the object plane, in which the field distribution, fall within the boundaries of the polygonal area, leave unchanged and sinulat outside its borders, and the process of iteration is repeated to obtain an undistorted image of the remote object.

 

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