CN114722223A - Astronomical image blind matching calculation method - Google Patents
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Abstract
The invention provides a blind matching calculation method for astronomical images, which comprises the steps of generating a theoretical star map according to a theoretical star table and sequencing the generated theoretical star map according to characteristics; calculating the position of each star map according to the sorted theoretical star maps to obtain an index table; and calculating the central direction and the pixel scale of the astronomical image according to the theoretical star map and the index table. The invention screens all-sky star tables, generates all-sky star map grids, has more uniform distribution of star maps and reduces the star map data quantity, improves the star map matching efficiency by manufacturing indexes through feature sorting, ensures that astronomical images can obtain the image center orientation under the condition of no prior information, improves the utilization rate of massive astronomical images by improving the condition that the observation data formats of different telescopes are not uniform and shared data is difficult to use and further saves a large amount of observation time and improves the working efficiency of astronomical researchers.
Description
Technical Field
The invention belongs to the technical field of astronomical image processing, and particularly relates to a blind matching calculation method for an astronomical image.
Background
The blind matching means that all prior information of an image is not known, and the prior information comprises but not limited to an image target surface, a pixel size, a telescope view field for shooting the image, an angular distance and an orientation, and information such as a central orientation, a pixel scale, an image rotation angle and the like of the image is calculated by matching according to star information of image shooting and star table data of a fixed star.
With the advent of the astronomical big data age, the number of astronomical images will grow exponentially. Most astronomical studies are performed using acquired astronomical images of a single telescope, which, although producing correct and standard metadata, the control systems of many telescopes drift with respect to the sky, producing only approximate celestial measurement metadata. Still other telescopes do not generate metadata, or generate metadata in some non-compliant form. Even with complex and highly automated measurements such as SDS, failures can occur in systems that generate celestial measurement calibration information, resulting in very good but unusable astronomical image data due to inefficient center pointing and pixel scale, resulting in inefficient use of such non-standard astronomical images, loss of significant observation time, and reduced work efficiency for astronomical researchers.
Disclosure of Invention
Aiming at the defects in the prior art, the invention provides a blind matching calculation method for astronomical images.
The invention provides a blind matching calculation method for astronomical images, which comprises the following steps:
and 3, calculating the center direction and the pixel scale of the astronomical image according to the theoretical star map and the index table.
Further, the generating the theoretical star map according to the theoretical star chart and sorting the generated theoretical star map according to the characteristics includes:
dividing a theoretical star catalogue into a plurality of grids according to the declination of the right ascension and the declination, and selecting the minimum star equivalent in the data of the theoretical star catalogue from each grid to generate a polygonal theoretical star map;
and (4) sequencing theoretical star maps at a maximum angle of 60-180 degrees and sequencing at a secondary maximum angle of 0-60 degrees.
Further, the calculating of the central direction and the pixel scale of the astronomical image according to the theoretical star map and the index table comprises the following steps:
301, acquiring the mass center and gray information of a point target in an astronomical image; the point target is an image spot of a fixed star in an astronomical image; the gray information comprises the pixel number of the point target, the length-width ratio of the point target and the gray sum of the point target;
step 302, sorting fixed stars in a descending order according to the number of pixels of the point target or the gray level of the point target to obtain an actual measurement star map;
step 303, performing polygon similarity matching on the actual measurement star map and the theoretical star map according to polygons formed by fixed stars to obtain a plurality of groups of matching constant star pairs;
step 304, calculating the pixel scale of the first group of matching constant star pairs, and finding out at least one group of matching constant star pairs with the same scale as the first group in the residual M-1 groups; wherein M is the number of groups matching the pair of constant stars; if the matching permanent star pair with the same scale as the first group can not be found in the rest M-1 groups; calculating the pixel scale of the second group of matching constant star pairs, and finding out at least one group of matching constant star pairs with the same scale as the second group from the rest M-2 groups; if the matching permanent star pair with the same scale as the second group can not be found in the rest M-2 group; calculating the pixel scale of the third group of matching permanent star pairs, and finding out at least one group of matching permanent star pairs with the same scale as the third group from the rest M-3 groups until the pixel scale of the M group of matching permanent star pairs is circularly calculated; if there are more than or equal to two groups of matching constant star pairs with the same pixel scale, calculating the six-constant negative film model coefficient;
305, calculating the center pointing direction and the rotation angle of the astronomical image according to the six-constant negative film model coefficient, and taking the pixel scale of the matched constant star pair with the same pixel scale as the pixel scale of the astronomical image;
step 306, carrying out full-map matching on a theoretical star catalogue and an actually measured fixed star according to the central direction, the image rotation angle and the pixel scale of the astronomical image;
step 307, judging whether the whole image matching meets a preset matching rate;
step 308, if yes, outputting the central direction, the image rotation angle and the pixel scale of the astronomical image;
if not, judging whether a matching constant star pair with the same pixel scale larger than or equal to the two groups exists according to the step 304;
if yes, go back to step 305;
if not; and determining the errors of the central direction, the image rotation angle and the pixel scale of the astronomical image, and exiting the calculation.
Further, the theoretical star catalogue is any one of GAIA star catalogue, Epigallograph, Digostar catalogue and FK5 star catalogue.
Further, the six-constant negative film model is:
wherein, (xi, zeta) is an ideal coordinate of a fixed star, and (x, y) is an image coordinate of the fixed star; a is a1Is a transverse equation constant term; b1And c1The coefficients are first order coefficients of a transverse equation; a is2Is a longitudinal equation constant term; b2And c2Are coefficients of the first order of the longitudinal equation.
Further, the obtaining an actually measured star map by sorting the stars in a descending order according to the number of pixels of the point target or the gray level of the point target includes:
setting star map characteristics; the star map features comprise polygons, main sequence star maps and vector maps;
setting a star map feature threshold; the star map feature threshold comprises a side length range, an angle range and the number of sides of the star map;
selecting a fixed star as a head end point, and selecting the fixed star from the remaining fixed stars to establish star map elements according to star map features and star map feature thresholds, wherein the star map elements are polygonal graphs, main sequence star maps or vector maps; the star map elements comprise point coordinates of all fixed stars of the star map, and characteristic values among all points, wherein the characteristic values comprise side lengths and angles;
selecting a plurality of fixed stars as head end points according to the star map characteristics to establish different star map elements;
sorting different star map elements according to the star map element characteristics to obtain an actually measured star map; the star map element characteristics comprise the length of each side and the angle of each corner of a polygonal graph, a main sequence star map or a vector map.
The invention provides a blind matching calculation method for astronomical images, which comprises the steps of generating a theoretical star map according to a theoretical star table and sequencing the generated theoretical star map according to characteristics; calculating the position of each star map according to the sorted theoretical star maps to obtain an index table; and calculating the center direction and the pixel scale of the astronomical image according to the theoretical star map and the index table. The invention screens the all-sky star catalogue and generates the all-sky star map grid, the distribution of star maps is more uniform and the data quantity of the star maps is reduced, the matching efficiency of the star maps is improved by making indexes through feature sorting, so that the astronomical images can obtain the central direction of the images under the condition of no prior information, and the pixel scale can improve the condition that the observation data formats of different telescopes are not uniform and the shared data is difficult to use, improve the utilization rate of massive astronomical images, further save a large amount of observation time and improve the working efficiency of astronomical researchers.
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In order to more clearly illustrate the technical solution of the present invention, the drawings needed to be used in the embodiments will be briefly described below, and it is obvious to those skilled in the art that other drawings can be obtained based on these drawings without creative efforts.
FIG. 1 is an astronomical image provided by an embodiment of the present invention;
fig. 2 is a flowchart of a method for computing an astronomical image blind matching according to an embodiment of the present invention;
FIG. 3 is a schematic diagram of a polygon constructed using star location geometry according to an embodiment of the present invention;
FIG. 4 is a schematic diagram of grid division according to an embodiment of the present invention;
fig. 5 is a Gaia DR2 source (star) density distribution diagram in the silver-trace coordinate system according to an embodiment of the present invention.
Detailed Description
The technical solutions in the embodiments of the present invention will be described clearly and completely with reference to the accompanying drawings in the embodiments of the present invention, and it is obvious that the described embodiments are only a part of the embodiments of the present invention, and not all of the embodiments. All other embodiments, which can be derived by a person skilled in the art from the embodiments given herein without making any creative effort, shall fall within the protection scope of the present invention.
As shown in fig. 1, the astronomical image is an image of observing a starry sky through a telescope, which images stars, planets, satellites and space debris in the night sky through the telescope onto a detector, typically a CCD or CMOS camera, mounted at the focus of the telescope. Fixed stars and targets generally present circular spots with a certain area due to point diffusion, coma may exist due to optical distortion of a telescope and the like, and the fixed stars and the targets may be stretched into ellipses due to different observation modes.
As shown in fig. 2, an embodiment of the present invention partially provides a method for computing blind matching of an astronomical image, including:
The theoretical star chart is a table book for recording various parameters of celestial bodies, such as positions, motions, stars and the like, spectrum types and the like. The formulation of star charts by astronomical observations is one of the very early works in astronomy. With the proposal of the observation principle of the middle-sky and the adoption of the novel telescope, the accuracy of the star catalogue is increasingly improved. The visual star tables commonly used in practical applications include GAIA star table, Epigallograph, Digita table, FK5 star table, etc.
As shown in fig. 5, the Gaia satellite can improve the measurement accuracy of the three-dimensional position of the celestial body obtained from the direction and parallax information and the tangential velocity obtained from the self-propelled data by more than 100 times, compared with the ebavalley satellite, and the equivalent angle measurement accuracy reaches the level of 10 micro-arcsec. Gaia is also increased many times over the observed target, with a total observed target well in excess of 10 hundred million celestial objects.
As shown in fig. 4, the theoretical star catalogue is divided into a target number of grids according to the declination of the right ascension and the declination, and the minimum star with the equivalent value in the data of the theoretical star catalogue is selected from each grid to generate a polygonal theoretical star catalogue. The star map is a graph constructed by using a star position geometric relationship, and generally comprises a triangle, a polygon, a vector star map and the like. The triangular star map is a simple and common star map, as shown in fig. 3, that is, any three stars are connected in the center. Generally, when a star map is established, the use times of each fixed star, the use times of each edge, the maximum edge length, the minimum edge length and the like are limited, so that the composition number is reduced, and the matching requirement can be met. The theoretical star map is a star map constructed by using a theoretical star chart, and the actual measurement star map is a star map established by using fixed stars in an astronomical observation image. When the two star maps are matched, the two star maps are converted to the same coordinate system.
The star position in the star catalogue is a coordinate taking the measuring center as the center under a celestial coordinate system, the coordinate (right ascension and declination) range is that the right ascension is 0-360 degrees, and the declination is-90 degrees. The grid division is to divide the projection of the fixed star on the celestial sphere according to a certain interval to form uniform grids. The mesh density may be divided as desired. The denser the grid, the smaller the scale of image pixels that can be detected, but the more voluminous the generated star map data, the slower the retrieval. In actual operation, grids of various specifications can be divided, solving is circularly called according to the sequence of pixel scale from large to small, and solving is quitted if solving is successful. The method not only ensures the resolving speed of the image with the larger pixel scale, but also considers the resolving capability of the small pixel scale, and ensures the efficiency and the success rate of the calculation.
When the telescope observes, the angle under the celestial coordinate system corresponding to each pixel is related to the telescope focal length, the view field size, the detector size and the like, and the angle corresponding to each pixel is a pixel scale. However, in the process of matching and solving, different pixel scales need to be classified and ordered, the different pixel scales are respectively solved, then the result calculated by each pixel scale is confirmed through actual measurement and theoretical star matching, and the result which is successfully matched is the final result.
And (3) carrying out two-stage sequencing on the triangular theoretical star map: the maximum angle is 60-180 degrees and the secondary maximum angle is 0-60 degrees. The purpose of sorting is to improve the matching speed, and the sorted star map sequence is stored according to a certain characteristic sequence.
And 2, calculating the position of each star map according to the sorted theoretical star maps to obtain an index table.
And 3, calculating the center direction and the pixel scale of the astronomical image according to the theoretical star map and the index table.
Step 301, processing an astronomical observation image by using an image processing software (Source Extractor) to acquire the mass center and gray information of a point target in the astronomical image; the point target is an image spot of a fixed star in an astronomical image; the gray information includes the number of pixels of the point object, the aspect ratio of the point object, and the sum of the gray of the point object.
And 302, sequencing the fixed stars in a descending order according to the pixel number of the point target or the gray scale of the point target to obtain the actually measured star map.
In the step, star map characteristics are set; the star map features comprise polygons, main sequence star maps and vector maps;
setting a star map feature threshold; the star map feature threshold comprises a side length range, an angle range and the number of sides of the star map;
selecting a fixed star as a head end point, selecting the fixed star from the remaining fixed stars according to the star map feature and the star map feature threshold to establish star map elements, wherein the star map elements are polygonal graphs, main sequence star maps or vector maps; the star map elements comprise point coordinates of all fixed stars of the star map, and characteristic values among all points, wherein the characteristic values comprise side lengths and angles;
selecting a plurality of fixed stars as head end points according to the star map characteristics to establish different star map elements;
sorting different star map elements according to the star map element characteristics to obtain an actually measured star map; the star map element characteristics comprise the length of each side and the angle of each corner of a polygonal graph, a main sequence star map or a vector map.
And 303, performing polygon similarity matching on the actual measurement star map and the theoretical star map according to polygons formed by fixed stars to obtain a plurality of groups of matching constant star pairs.
Step 304, calculating the pixel scale of the first group of matching constant star pairs, and finding out at least one group of matching constant star pairs with the same scale as the first group in the residual M-1 groups; wherein M is the number of groups matching the pair of constant stars; if the matching permanent star pair with the same scale as the first group can not be found in the rest M-1 groups; calculating the pixel scale of the second group of matching constant star pairs, and finding out at least one group of matching constant star pairs with the same scale as the second group from the rest M-2 groups; if the matching permanent star pair with the same scale as the second group can not be found in the rest M-2 group; calculating the pixel scale of the third group of matching permanent star pairs, and finding out at least one group of matching permanent star pairs with the same scale as the third group from the rest M-3 groups until the pixel scale of the M group of matching permanent star pairs is circularly calculated; if there are more than or equal to two groups of matching constant star pairs with the same pixel scale, calculating the six-constant negative film model coefficient.
And 305, calculating the central direction and the image rotation angle of the astronomical image according to the six-constant negative film model coefficient, and taking the pixel scale of the matched constant star pair with the same pixel scale as the pixel scale of the astronomical image.
The six-constant negative film model is as follows:
wherein, (xi, zeta) is an ideal coordinate of a fixed star, and (x, y) is an image coordinate of the fixed star; a is1Is a constant term of a transverse equation; b1And c1The coefficients are first order coefficients of a transverse equation; a is2Is a longitudinal equation constant term; b2And c2Are coefficients of the first order of the longitudinal equation.
Step 306, carrying out full-map matching on a theoretical star catalogue and an actually measured fixed star according to the central direction, the image rotation angle and the pixel scale of the astronomical image;
step 307, judging whether the whole image matching meets a preset matching rate;
step 308, if yes, outputting the central direction, the image rotation angle and the pixel scale of the astronomical image;
if not, judging whether a matching constant star pair with the same pixel scale larger than or equal to the two groups exists according to the step 304;
if yes, go back to step 305;
if not; and determining the errors of the central direction, the image rotation angle and the pixel scale of the astronomical image, and exiting the calculation.
The center pointing is that the image center coordinate corresponds to the declination value of the right ascension under the celestial coordinate system, and if the image is p × q, the coordinate is
Namely the image center, the corresponding declination value of the declination in the celestial coordinate system is an angle (alpha, delta), the image can be clearly known to have the fixed stars in the image through the value, namely the pixel scale, and the position of the fixed stars in the image can be located, so that a fixed star position image projected to an observed image from a theoretical star table can be obtained, the image and an actual observed image can be completely aligned through rotation, the same fixed stars are located at the same position in the observed image, but because the telescope detection capability and the actual measured star image cannot completely contain the fixed stars in the theoretical star table, because some fixed stars are too far and too dark, and the aperture of the telescope is too small to see. The matching does not need to match all stars, but only needs a part of the matching. If the requirement of matching is not met, the matching is wrong, and the opposite is correct.
The invention has been described in detail with reference to specific embodiments and illustrative examples, but the description is not intended to be construed in a limiting sense. Those skilled in the art will appreciate that various equivalent substitutions, modifications or improvements may be made to the technical solution of the present invention and its embodiments without departing from the spirit and scope of the present invention, which fall within the scope of the present invention. The scope of the invention is defined by the appended claims.
Claims (6)
1. An astronomical image blind matching calculation method is characterized by comprising the following steps:
step 1, generating a theoretical star map according to a theoretical star table and sequencing the generated theoretical star map according to characteristics;
step 2, calculating the position of each star map according to the sorted theoretical star maps to obtain an index table;
and 3, calculating the center direction and the pixel scale of the astronomical image according to the theoretical star map and the index table.
2. The astronomical image blind matching calculation method of claim 1, wherein the generating of the theoretical star map from the theoretical star table and sorting the generated theoretical star map by features comprises:
dividing a theoretical star catalogue into a plurality of grids according to the declination of the right ascension and the declination, and selecting the minimum star equivalent in the data of the theoretical star catalogue from each grid to generate a polygonal theoretical star map;
and (4) sequencing theoretical star maps at a maximum angle of 60-180 degrees and sequencing at a secondary maximum angle of 0-60 degrees.
3. The astronomical image blind matching calculation method according to claim 1, wherein the calculating of the central direction and the pixel scale of the astronomical image according to the theoretical star map and the index table comprises:
step 301, acquiring centroid and gray information of a point target in an astronomical image; the point target is an image spot of a fixed star in an astronomical image; the gray information comprises the pixel number of the point target, the length-width ratio of the point target and the gray sum of the point target;
step 302, sorting fixed stars in a descending order according to the number of pixels of the point target or the gray level of the point target to obtain an actual measurement star map;
step 303, performing polygon similarity matching on the actual measurement star map and the theoretical star map according to polygons formed by fixed stars to obtain a plurality of groups of matching constant star pairs;
step 304, calculating the pixel scale of the first group of matching constant star pairs, and finding out at least one group of matching constant star pairs with the same scale as the first group in the residual M-1 groups; wherein M is the number of groups matching the pair of constant stars; if the matching permanent star pair with the same scale as the first group can not be found in the rest M-1 groups; calculating the pixel scale of the second group of matching constant star pairs, and finding out at least one group of matching constant star pairs with the same scale as the second group from the rest M-2 groups; if the matching constant star pair with the same scale as the second group cannot be found in the rest M-2 group; calculating the pixel scale of the third group of matching permanent star pairs, and finding out at least one group of matching permanent star pairs with the same scale as the third group from the rest M-3 groups until the pixel scale of the M group of matching permanent star pairs is circularly calculated; if there are more than or equal to two groups of matching constant star pairs with the same pixel scale, calculating the six-constant negative film model coefficient;
305, calculating the center pointing direction and the rotation angle of the astronomical image according to the six-constant negative film model coefficient, and taking the pixel scale of the matched constant star pair with the same pixel scale as the pixel scale of the astronomical image;
step 306, carrying out full-map matching on a theoretical star catalogue and an actually measured fixed star according to the central direction, the image rotation angle and the pixel scale of the astronomical image;
step 307, judging whether the whole image matching meets a preset matching rate;
step 308, if yes, outputting the central direction, the image rotation angle and the pixel scale of the astronomical image;
if not, judging whether a matching constant star pair with the same pixel scale larger than or equal to two groups exists according to the step 304;
if yes, go back to step 305;
if not; and determining the errors of the central direction, the image rotation angle and the pixel scale of the astronomical image, and exiting the calculation.
4. The astronomical image blind matching calculation method of claim 1, wherein the theoretical star table is any one of a GAIA star table, an eba star table, a valley star table and an FK5 star table.
5. The astronomical image blind matching calculation method of claim 4, wherein the six-constant negative model is:
wherein, (xi, zeta) is an ideal coordinate of a fixed star, and (x, y) is an image coordinate of the fixed star; a is1Is a constant term of a transverse equation; b1And c1The coefficients are first order coefficients of a transverse equation; a is2Is a longitudinal equation constant term; b2And c2Are coefficients of the first order of the longitudinal equation.
6. The astronomical image complete-blind matching calculation method of claim 3, wherein the step of obtaining the actually measured star map by sorting the stars in a descending order according to the number of pixels of the point target or the gray scale of the point target comprises the following steps:
setting star map characteristics; the star map features comprise polygons, main sequence star maps and vector maps;
setting a star map feature threshold; the star map feature threshold comprises a side length range, an angle range and the number of sides of the star map;
selecting a fixed star as a head end point, and selecting the fixed star from the remaining fixed stars to establish star map elements according to star map features and star map feature thresholds, wherein the star map elements are polygonal graphs, main sequence star maps or vector maps; the star map elements comprise point coordinates of all fixed stars of the star map, and characteristic values among all points, wherein the characteristic values comprise side lengths and angles;
selecting a plurality of fixed stars as head end points according to the star map characteristics to establish different star map elements;
sorting different star map elements according to the star map element characteristics to obtain an actually measured star map; the star map element characteristics comprise the length of each side and the angle of each corner of a polygonal graph, a main sequence star map or a vector map.
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| CN115356777A (en) * | 2022-08-23 | 2022-11-18 | 中国科学院云南天文台 | Method for searching maximum observation signal of celestial body measurement type micro-gravity lens event and star-to-nearest moment |
| CN117308889A (en) * | 2023-09-22 | 2023-12-29 | 广东海洋大学 | High-precision celestial body measuring method for all chip units of joint spliced CCD |
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Cited By (3)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN115356777A (en) * | 2022-08-23 | 2022-11-18 | 中国科学院云南天文台 | Method for searching maximum observation signal of celestial body measurement type micro-gravity lens event and star-to-nearest moment |
| CN117308889A (en) * | 2023-09-22 | 2023-12-29 | 广东海洋大学 | High-precision celestial body measuring method for all chip units of joint spliced CCD |
| CN117308889B (en) * | 2023-09-22 | 2024-04-02 | 广东海洋大学 | High-precision celestial body measuring method for all chip units of joint spliced CCD |
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