Method, device, equipment and medium for detecting the limit detection capability of ground-based optical telescope

Abstract

The present invention relates to the field of astronomical observation, and provides a detection method, device, equipment and medium for the limit detection capability of a ground-based optical telescope. The method comprises: acquiring a target image through an optical telescope; extracting a plurality of measurement stars on the target image, and calculating the measurement magnitude of each measurement star; using a cross-matching algorithm, cross-matching each measurement star with a pre-configured reference star catalog to obtain successfully matched matching stars, and the measurement magnitude and reference magnitude corresponding to the matching star, wherein the reference magnitude is the magnitude given by the reference star catalog; calculating the linearity between the measurement magnitude and the reference magnitude of the matching star, and eliminating the mismatched stars in the matching stars according to the linearity to obtain the detection stars; comparing the reference magnitudes of the detection stars, and selecting the maximum value of the reference magnitudes of the detection stars as the limit detection magnitude.

Description

Technical Field

[0001] The present invention relates to the field of astronomical observation, and in particular to a method, device, equipment and storage medium for detecting the limit detection capability of a ground-based optical telescope. Background Art

[0002] The ultimate detection capability of ground-based optical telescopes is affected by environmental factors such as the atmospheric seeing at the observation site. Specifically, factors such as the temperature gradient, humidity changes, wind speed and wind direction fluctuations in the atmosphere will cause light to refract and scatter when passing through the atmosphere, thereby reducing the accuracy of the observation data. Therefore, even for the same telescope, when it is moved to different observation stations, its ultimate detection capability will vary due to different atmospheric conditions in different places. This means that after the telescope is moved to the new site, its detection capability must be re-measured in detail to ensure the scientificity and effectiveness of subsequent observations. In addition, as the use time of ground-based optical telescopes increases, the optical devices in them age and the ultimate detection capability decreases accordingly. Therefore, in order to maintain the observation accuracy and efficiency of the telescope, its detection capability must be recalibrated regularly after the telescope has been in operation for a period of time, so as to better arrange astronomical observation plans and improve observation efficiency, and to promptly detect possible problems with the telescope. Summary of the invention

[0003] 1. Technical issues to be resolved

[0004] In view of the above problems, the present invention provides a method, device, equipment and storage medium for detecting the limit detection capability of a ground-based optical telescope, so as to at least partially solve the technical problems such as reduced accuracy of observation data of optical telescopes, reduced scientificity and effectiveness of observations, etc.

[0005] (II) Technical solution

[0006] The present invention provides a method for detecting the limit detection capability of a ground-based optical telescope, comprising: acquiring a target image through an optical telescope; extracting a plurality of measurement stars on the target image, and calculating the measurement magnitude of each measurement star; using a cross-matching algorithm, cross-matching each measurement star with a pre-configured reference star catalog to obtain successfully matched matching stars, and the measurement magnitude and reference magnitude corresponding to the matching stars, wherein the reference magnitude is the magnitude given by the reference star catalog; calculating the linearity between the measurement magnitude and the reference magnitude of the matching stars, and eliminating mismatched stars from the matching stars according to the linearity to obtain detection stars; comparing the reference magnitudes of the detection stars, and selecting the maximum value of the reference magnitudes of the detection stars as the limit detection magnitude.

[0007] According to an embodiment of the present invention, the method further includes: calculating a standard deviation of a reference magnitude corresponding to the matching stars; and based on the standard deviation, eliminating matching stars whose reference magnitude is greater than a first preset value.

[0008] According to an embodiment of the present invention, configuring the reference star catalog includes: performing astronomical positioning on the measured stars, calculating the celestial coordinates of the center position of the target image and the measured stars; and acquiring the reference star catalog based on the celestial coordinates and the detection field of view of the optical telescope.

[0009] According to an embodiment of the present invention, the linearity between the measured magnitude and the reference magnitude of the matching stars is calculated, and the mismatched stars in the matching stars are eliminated according to the linearity to obtain the detected stars, including: using a scatter plot to visualize the measured magnitude and the reference magnitude of each matching star, and selecting a data segment in the scatter plot whose linearity is greater than a second preset value; performing linear fitting on the data segment to obtain a linear equation and a corresponding linear fitting line; calculating the vertical distance between each scatter point in the scatter plot and the linear fitting line, and eliminating the scatter points whose vertical distance is greater than a threshold value to eliminate the mismatched stars in the matching stars, and obtain the detected stars.

[0010] According to an embodiment of the present invention, the method further comprises: for the target image, performing at least image preprocessing of background correction, flat field correction, dark field subtraction, bad pixel processing and cosmic ray processing.

[0011] According to an embodiment of the present invention, the field of view of the reference star catalog is larger than the detection field of view of the optical telescope.

[0012] According to an embodiment of the present invention, acquiring a target image through an optical telescope includes: using the optical telescope to acquire the target image through background measurement, dark field measurement, flat field measurement and stargazing measurement.

[0013] The second aspect of the present invention provides a detection device for the limit detection capability of a ground-based optical telescope, comprising: an acquisition module, used to acquire a target image through an optical telescope; an extraction module, used to extract multiple measurement stars on the target image, and calculate the measurement magnitude of each measurement star; a matching module, used to cross-match each measurement star with a pre-configured reference star catalog using a cross-matching algorithm, to obtain successfully matched matching stars, and the measurement magnitude and reference magnitude corresponding to the matching stars, wherein the reference magnitude is the magnitude given by the reference star catalog; a elimination module, used to calculate the linearity of the measurement magnitude and the reference magnitude of the matching stars, and eliminate the mismatched stars in the matching stars according to the linearity to obtain the detection stars; a determination module, used to compare the reference magnitudes of the detection stars, and select the maximum value of the reference magnitudes of the detection stars as the limit detection magnitude.

[0014] The third aspect of the present invention provides an electronic device, comprising: one or more processors; a storage device for storing one or more computer programs, when the one or more programs are executed by the one or more processors, the one or more processors execute the method for detecting the limit detection capability of the ground-based optical telescope.

[0015] The fourth aspect of the present invention also provides a computer-readable storage medium having executable instructions stored thereon, which, when executed by a processor, causes the processor to execute the method for detecting the limit detection capability of a ground-based optical telescope.

[0016] (III) Beneficial effects

[0017] The detection method, device, equipment and storage medium of the limit detection capability of the ground-based optical telescope provided by the present invention eliminate mismatched stars, complete high-precision outlier elimination processing, and obtain real matching data, thereby calibrating the detection capability of the ground-based optical telescope, improving the accuracy of the observation data, as well as the scientificity and effectiveness of the observation, so as to better arrange astronomical observations. BRIEF DESCRIPTION OF THE DRAWINGS

[0018] For a more complete understanding of the present invention and its advantages, reference will now be made to the following description taken in conjunction with the accompanying drawings, in which:

[0019] Figure 1 The flowchart of the method for detecting the limit detection capability of a ground-based optical telescope provided by an embodiment of the present invention is schematically shown;

[0020] Figure 2 A schematic diagram of a star catalog matching result distribution diagram provided by an embodiment of the present invention is shown;

[0021] Figure 3A schematic diagram of stars in a reference star catalog and a target image provided by an embodiment of the present invention is schematically shown;

[0022] Figure 4 A schematic diagram of the limit detection magnitude provided by an embodiment of the present invention is schematically shown;

[0023] Figure 5 A schematic diagram showing a structural block diagram of a device for detecting the limit detection capability of a ground-based optical telescope provided in accordance with an embodiment of the present invention;

[0024] Figure 6 The hardware structure diagram of an electronic device is schematically shown. DETAILED DESCRIPTION

[0025] Below, embodiments of the present invention will be described with reference to the accompanying drawings. However, it should be understood that these descriptions are exemplary only and are not intended to limit the scope of the present invention. In the following detailed description, for ease of explanation, many specific details are set forth to provide a comprehensive understanding of embodiments of the present invention. However, it is apparent that one or more embodiments may also be implemented without these specific details. In addition, in the following description, descriptions of known structures and technologies are omitted to avoid unnecessary confusion of concepts of the present invention.

[0026] The terms used herein are only for describing specific embodiments and are not intended to limit the present invention. The terms "comprise", "include", etc. used herein indicate the existence of the features, steps, operations and / or components, but do not exclude the existence or addition of one or more other features, steps, operations or components.

[0027] All terms (including technical and scientific terms) used herein have the meanings commonly understood by those skilled in the art unless otherwise defined. It should be noted that the terms used herein should be interpreted as having a meaning consistent with the context of this specification and should not be interpreted in an idealized or overly rigid manner.

[0028] Some block diagrams and / or flow charts are shown in the accompanying drawings. It should be understood that some blocks or combinations thereof in the block diagrams and / or flow charts may be implemented by computer program instructions. These computer program instructions may be provided to a processor of a general-purpose computer, a special-purpose computer, or other programmable data processing device, so that these instructions, when executed by the processor, may create a device for implementing the functions / operations described in these block diagrams and / or flow charts.

[0029] Therefore, the technology of the present invention can be implemented in the form of hardware and / or software (including firmware, microcode, etc.). In addition, the technology of the present invention can take the form of a computer program product on a computer-readable medium storing instructions, which can be used by an instruction execution system or in combination with an instruction execution system. In the context of the present invention, a computer-readable medium can be any medium that can contain, store, transmit, propagate or transmit instructions. For example, a computer-readable medium can include, but is not limited to, an electrical, magnetic, optical, electromagnetic, infrared or semiconductor system, device, device or propagation medium. Specific examples of computer-readable media include: magnetic storage devices, such as magnetic tape or hard disk (HDD); optical storage devices, such as compact disk (CD-ROM); memory, such as random access memory (RAM) or flash memory; and / or wired / wireless communication links.

[0030] like Figure 1 As shown, the flowchart of the method for detecting the limit detection capability of a ground-based optical telescope includes S1 to S5.

[0031] In operation S1 , a target image is acquired through an optical telescope.

[0032] In operation S2, a plurality of measurement stars on the target image are extracted, and the measurement magnitude of each of the measurement stars is calculated.

[0033] In operation S3, a cross-matching algorithm is used to cross-match each of the measured stars with a pre-configured reference star catalog to obtain successfully matched matching stars, as well as the measured magnitude and reference magnitude corresponding to the matching stars, wherein the reference magnitude is the magnitude given by the reference star catalog.

[0034] In operation S4, the linearity between the measured magnitude of the matching star and the reference magnitude is calculated, and the mismatched stars in the matching stars are eliminated according to the linearity to obtain the detected stars.

[0035] In operation S5, the reference magnitudes of the detected stars are compared, and the maximum value of the reference magnitudes of the detected stars is selected as the limiting detection magnitude.

[0036] Specifically, acquiring the target image through the optical telescope includes: using the optical telescope to acquire the target image through background measurement, dark field measurement, flat field measurement and stargazing measurement.

[0037] Exemplarily, a photometric night is selected for image acquisition. The environment requires a clear, cloudless sky, no moon, a wind speed of less than 5m / s, skylight better than 20mV / arcsec2, and the seeing of the observation station should be better than the local average seeing. Image acquisition methods include background measurement images, dark field measurement images, flat field measurement images, and stargazing images. Among them, the background measurement image is taken in a dark environment, the dome is closed, the lens cover is closed, and the minimum exposure time is set for shooting. The dark field measurement image is taken in a dark environment, the dome is closed, the lens cover is closed, and the exposure time is set to be consistent with the exposure time of the stargazing image. The flat field measurement image refers to the dome being opened and the lens cover being opened before the observation, and the flat field light in the dome is taken. If there is no flat field light, the sky can be shot at the beginning of dawn or the end of dusk, and the exposure time is set to be consistent with the exposure time of the stargazing image. The stargazing image is taken with the dome open, the lens cover open, and the sky is observed in the stargazing mode. The exposure time is set according to the measurement requirements.

[0038] On the basis of the above embodiments, in this embodiment, for the target image, at least background correction, flat field correction, dark field subtraction, bad pixel processing and cosmic ray processing are performed as image preprocessing, and the bright stars on the image, i.e., the measured stars, can be extracted by threshold detection method. These stars are the stars actually observed by the telescope, and their brightness, position, quantity and other information will be used for cross-matching and comparison with the reference star catalog. Then, the flow data and pixel coordinates of the measured stars are calculated, and the measured magnitude of the measured stars is calculated based on the flow data.

[0039] Furthermore, by setting the matching threshold, the measured stars can be cross-matched with the reference stars in the pre-configured high-precision reference star catalog using the cross-matching algorithm and the star catalog matching method. At the same time, the successfully matched stars and their reference magnitudes and measured magnitudes are counted, such as Figure 2 shown.

[0040] It can be understood that by extracting multiple measured stars on the target image, calculating their measured magnitudes, and then cross-matching them with the pre-configured reference star catalog, the accuracy of star identification can be significantly improved. Among them, the cross-matching algorithm helps to eliminate misidentified stars, thereby ensuring the accuracy of subsequent analysis.

[0041] Configuring the reference star catalog includes: performing astronomical positioning on the measured star, calculating the center position of the target image and the celestial coordinates of the measured star; and obtaining the reference star catalog based on the celestial coordinates and the detection field of view of the optical telescope.

[0042] In some exemplary embodiments, the parameters of the measured stars extracted by the above embodiments are used to call the astronomical image calibration tool for astronomical positioning to obtain the world coordinate system parameters. Then, the coordinates (x0, y0) at the center of the image and the extracted star coordinates (x, y) are converted into celestial coordinates (RA, DEC) using the world coordinate system parameters. Then, the corresponding reference star catalog is obtained based on the right ascension and declination of the center of the image and the detection field of view of the telescope.

[0043] It should be noted that in order to ensure the completeness of the stars in the field of view, the field of view of the reference star catalog should be slightly larger than the detection field of the optical telescope. At the same time, the depth of the reference star catalog should be large enough, that is, larger than the theoretical detection limit of the telescope, and take into account the actual observation conditions, such as atmospheric transparency, the altitude of the observation site, and the observation efficiency of the telescope.

[0044] Figure 3 A schematic diagram of a reference star catalog and stars in a target image provided by an embodiment of the present invention is schematically shown.

[0045] like Figure 3 As shown, the reference catalog stars, represented by dots, are plotted within a larger circular field of view, which is slightly larger than the detection field of view of an optical telescope. The measured stars in the target image are plotted within a smaller detection field of view, represented by square marks.

[0046] It is understandable that the field of view of the reference star catalog is slightly larger than the actual detection field of view of the optical telescope, which helps to reduce the omission of stars caused by insufficient field of view, thereby improving the accuracy and reliability of the detection results. At the same time, it can also reduce the impact of possible aberrations and distortions at the edge of the detection field on the detection results.

[0047] The real star data after matching is processed with high precision to eliminate mismatched star sources. Finally, the magnitude of the faintest star, that is, the maximum value of the reference magnitude, is selected as the limiting detection magnitude to characterize the telescope's limiting detection capability.

[0048] It can be understood that by calculating the linearity between the measured magnitude of the matching star and the reference magnitude, and eliminating the mismatched stars accordingly, the error introduced by the mismatch is effectively reduced, ensuring the stability and reliability of the matching result. Therefore, the method provided by the embodiment of the present invention has strong adaptability and can be applied not only to the index detection of newly manufactured optical telescopes, but also to the calibration of telescopes in use, so as to better use the telescopes for astronomical observations.

[0049] In an embodiment of the present invention, the method further includes: calculating a standard deviation of a reference magnitude corresponding to the matching stars; and based on the standard deviation, eliminating matching stars whose reference magnitude is greater than a first preset value.

[0050] Specifically, the standard deviation σ of the reference magnitude of the successfully matched stars is calculated, and the stars whose reference magnitude is greater than three times the standard deviation 3σ are eliminated using the 3σ principle. Before the mismatched stars in the matching stars are eliminated based on linearity, the first outlier elimination process is completed.

[0051] The formula for calculating standard deviation is:

[0052] Among them, x is the reference magnitude of each matching star, μ is the average reference magnitude of all matching stars, and N is the number of matching stars.

[0053] It is understandable that stars with reference magnitudes greater than three standard deviations 3σ may have abnormal magnitude values ​​due to observational errors, data processing errors or other reasons, so removing them can improve the accuracy and reliability of subsequent analysis.

[0054] On the basis of the above embodiments, in this embodiment, the linearity between the measured magnitude and the reference magnitude of the matching stars is calculated, and the mismatched stars in the matching stars are eliminated according to the linearity to obtain the detected stars, including: using a scatter plot to visualize the measured magnitude and the reference magnitude of each matching star, and selecting a data segment in the scatter plot whose linearity is greater than a second preset value; performing linear fitting on the data segment to obtain a linear equation and a corresponding linear fitting line; calculating the vertical distance between each scatter point in the scatter plot and the linear fitting line, and eliminating the scatter points whose vertical distance is greater than a threshold value to eliminate the mismatched stars in the matching stars, and obtain the detected stars.

[0055] The reference magnitude and measured magnitude of the successfully matched stars show an obvious linear relationship. A magnitude range with good linearity is selected for linear fitting to obtain a first-order equation. By calculating the vertical distance from each point to the line, scattered points with large distance values, that is, scattered points with a large degree of dispersion, are eliminated, thereby eliminating the mismatched stars, obtaining the detected stars, and completing the abnormal point elimination process.

[0056] For example, a magnitude range with good linearity is selected (e.g. Figure 2The measured magnitudes of the stars with reference magnitudes of 11 to 14 are linearly fitted to obtain a linear fitting equation. Then, the degree of dispersion of the data points in the graph is calculated by calculating the vertical distance from the star to the straight line, and the scattered points with large dispersion are eliminated. On the basis of eliminating the mismatched stars based on the standard deviation, the second outlier elimination process is completed, thereby further eliminating the mismatched stars.

[0057] Figure 4 The diagram schematically shows a schematic diagram of the limit detection magnitude provided by an embodiment of the present invention.

[0058] like Figure 4 As shown, at the top of the fitting curve, the reference magnitude of the limiting star is slightly greater than 16, which is the limiting detection magnitude of the telescope.

[0059] Based on the above-mentioned detection method of the limit detection capability of the ground-based optical telescope, the present invention also provides a detection device for the limit detection capability of the ground-based optical telescope. Figure 5 The device is described in detail.

[0060] like Figure 5 As shown, the detection device 500 of the limit detection capability of the ground-based optical telescope in this embodiment includes an acquisition module 501, an extraction module 502, a matching module 503, a elimination module 504 and a determination module 505.

[0061] The acquisition module 501 is used to acquire a target image through an optical telescope.

[0062] The extraction module 502 is used to extract a plurality of measured stars on the target image and calculate the measured magnitude of each of the measured stars.

[0063] The matching module 503 is used to cross-match each of the measured stars with a pre-configured reference star catalog using a cross-matching algorithm to obtain successfully matched matching stars, as well as the measured magnitude and reference magnitude corresponding to the matching stars, wherein the reference magnitude is the magnitude given by the reference star catalog.

[0064] The elimination module 504 is used to calculate the linearity between the measured magnitude of the matching stars and the reference magnitude, and eliminate the mismatched stars in the matching stars according to the linearity to obtain the detected stars.

[0065] The determination module 505 is used to compare the reference magnitudes of the detected stars and select the maximum value of the reference magnitudes of the detected stars as the limiting detection magnitude.

[0066] It is understandable that the acquisition module 501, the extraction module 502, the matching module 503, the elimination module 504 and the determination module 505 can be combined in one module for implementation, or any one of the modules can be split into multiple modules. Alternatively, at least part of the functions of one or more of these modules can be combined with at least part of the functions of other modules and implemented in one module. According to an embodiment of the present invention, at least one of the acquisition module 501, the extraction module 502, the matching module 503, the elimination module 504 and the determination module 505 can be at least partially implemented as a hardware circuit, such as a field programmable gate array (FPGA), a programmable logic array (PLA), a system on a chip, a system on a substrate, a system on a package, an application specific integrated circuit (ASIC), or can be implemented in hardware or firmware such as any other reasonable way of integrating or packaging the circuit, or in a suitable combination of software, hardware and firmware. Alternatively, at least one of the acquisition module 501, the extraction module 502, the matching module 503, the elimination module 504 and the determination module 505 may be at least partially implemented as a computer program module, and when the program is executed by a computer, the function of the corresponding module may be executed.

[0067] Figure 6 The structure block diagram of an electronic device provided by an embodiment of the present invention is schematically shown.

[0068] like Figure 6 As shown, the electronic device described in this embodiment includes: the electronic device 600 includes a processor 610 and a computer readable storage medium 620. The electronic device 600 can execute the above reference Figure 1 Describes the method to achieve detection of specific operations.

[0069] Specifically, the processor 610 may include, for example, a general-purpose microprocessor, an instruction set processor and / or a related chipset and / or a dedicated microprocessor (e.g., an application-specific integrated circuit (ASIC)), etc. The processor 610 may also include an onboard memory for cache purposes. The processor 610 may be a processor for executing reference Figure 1 The described method flow according to the embodiment of the present invention may be a single processing unit or multiple processing units for different actions.

[0070] Computer readable storage medium 620, for example, can be any medium capable of containing, storing, conveying, propagating or transmitting instructions. For example, readable storage media can include, but are not limited to, electronic, magnetic, optical, electromagnetic, infrared or semiconductor systems, devices, devices or propagation media. Specific examples of readable storage media include: magnetic storage devices, such as magnetic tapes or hard disks (HDDs); optical storage devices, such as compact disks (CD-ROMs); memory, such as random access memory (RAM) or flash memory; and / or wired / wireless communication links.

[0071] The computer readable storage medium 620 may include a computer program 621, which may include code / computer executable instructions, which when executed by the processor 610 causes the processor 610 to perform, for example, the above-mentioned combination Figure 1 The described method sequences and any variations thereof.

[0072] The computer program 621 may be configured to have, for example, computer program codes including computer program modules. For example, in an exemplary embodiment, the codes in the computer program 621 may include one or more program modules, for example, including 621A, module 621B, ... It should be noted that the division method and number of modules are not fixed, and those skilled in the art may use appropriate program modules or program module combinations according to actual conditions. When these program module combinations are executed by the processor 610, the processor 610 may execute, for example, the above combination of Figure 1~Figure 4 The described method sequences and any variations thereof.

[0073] According to an embodiment of the present invention, at least one of the acquisition module 501, the extraction module 502, the matching module 503, the elimination module 504 and the determination module 505 can be implemented as a reference. Figure 6 The computer program modules described herein, when executed by the processor 610, can implement the corresponding operations described above.

[0074] The present invention also provides a computer-readable medium, which may be included in the device / apparatus / system described in the above embodiment; or may exist independently without being assembled into the device / apparatus / system. The above computer-readable medium carries one or more programs, and when the above one or more programs are executed, the method according to the embodiment of the present invention is implemented.

[0075] It will be appreciated by those skilled in the art that the features described in the various embodiments of the present invention may be combined and / or combined in various ways, even if such combinations or combinations are not explicitly described in the present invention. In particular, without departing from the spirit and teachings of the present invention, the features described in the various embodiments of the present invention may be combined and / or combined in various ways. All of these combinations and / or combinations fall within the scope of the present invention.

[0076] The specific embodiments described above further illustrate the objectives, technical solutions and beneficial effects of the present invention in detail. It should be understood that the above description is only a specific embodiment of the present invention and is not intended to limit the present invention. Any modifications, equivalent substitutions, improvements, etc. made within the spirit and principles of the present invention should be included in the protection scope of the present invention.

Claims

1. A method for detecting the limit detection capability of a ground-based optical telescope, characterized in that: include: Acquire target images through optical telescopes; Extracting a plurality of measured stars on the target image, and calculating the measured magnitude of each of the measured stars; Using a cross-matching algorithm, cross-match each of the measured stars with a pre-configured reference star catalog to obtain successfully matched matching stars, and the measured magnitude and reference magnitude corresponding to the matching stars, wherein the reference magnitude is the magnitude given by the reference star catalog; The measured magnitude and reference magnitude of each matching star are visualized using a scatter plot, and a data segment whose linearity is greater than a second preset value in the scatter plot is selected; a linear fit is performed on the data segment to obtain a linear equation and a corresponding linear fitting line; a vertical distance between each scattered point in the scatter plot and the linear fitting line is calculated, and scattered points whose vertical distance is greater than a threshold are eliminated to eliminate mismatched stars from the matching stars, thereby obtaining detected stars; The reference magnitudes of the detected stars are compared, and the maximum value of the reference magnitudes of the detected stars is selected as the limiting detection magnitude.

2. The method for detecting the limit detection capability of a ground-based optical telescope according to claim 1, characterized in that: The method further comprises: Calculate the standard deviation of the reference magnitude corresponding to the matching star; Based on the standard deviation, matching stars whose reference magnitude is greater than a first preset value are eliminated.

3. The method for detecting the limit detection capability of a ground-based optical telescope according to claim 1, characterized in that: Configuring the reference star catalog includes: Performing astronomical positioning on the measured star, and calculating the celestial coordinates of the center position of the target image and the measured star; The reference star catalog is acquired based on the celestial coordinates and the detection field of view of the optical telescope.

4. The method for detecting the limit detection capability of a ground-based optical telescope according to claim 1, characterized in that: The method further comprises: For the target image, at least image preprocessing including background correction, flat field correction, dark field subtraction, bad pixel processing and cosmic ray processing is performed.

5. The method for detecting the limit detection capability of a ground-based optical telescope according to claim 3, characterized in that: The field of view of the reference star catalog is larger than the detection field of view of the optical telescope.

6. The method for detecting the limit detection capability of a ground-based optical telescope according to claim 1, characterized in that: Acquiring target images through optical telescopes includes: The target image is acquired by using the optical telescope through background measurement, dark field measurement, flat field measurement and stargazing measurement.

7. A device for detecting the limit detection capability of a ground-based optical telescope, characterized in that: The device comprises: An acquisition module, used for acquiring a target image through an optical telescope; An extraction module, used for extracting a plurality of measured stars on the target image and calculating the measured magnitude of each of the measured stars; A matching module, used to cross-match each of the measured stars with a pre-configured reference star catalog by using a cross-matching algorithm to obtain successfully matched matching stars, and the measured magnitude and reference magnitude corresponding to the matching stars, wherein the reference magnitude is the magnitude given by the reference star catalog; A rejection module is used to visualize the measured magnitude and reference magnitude of each of the matching stars using a scatter plot, and select a data segment in the scatter plot whose linearity is greater than a second preset value; perform linear fitting on the data segment to obtain a linear equation and a corresponding linear fitting line; calculate the vertical distance between each scatter point in the scatter plot and the linear fitting line, and reject the scatter points whose vertical distance is greater than a threshold value, so as to reject the mismatched stars in the matching stars and obtain the detected stars; The determination module is used to compare the reference magnitudes of the detected stars and select the maximum value of the reference magnitudes of the detected stars as the limiting detection magnitude.

8. An electronic device, comprising: one or more processors; a storage device for storing one or more computer programs, It is characterized in that when the one or more programs are executed by the one or more processors, the one or more processors execute the method according to any one of claims 1 to 6.

9. A computer-readable storage medium having executable instructions stored thereon, characterized in that: When the instruction is executed by a processor, the processor executes the method according to any one of claims 1 to 6.

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