Astronomical telescope imaging detection capability evaluation method, device, equipment and medium

Abstract

The invention discloses an astronomical telescope imaging detection capability evaluation method, device and equipment and a medium, and relates to the field of space optical system ground testing, and the method comprises the steps: taking a point source image peak value of point source image blocks obtained based on a simulation light source as a center, and carrying out the superposition of all point source image blocks, and obtaining a target point source image block; splitting the target point source image block into a point source region and a point source background region, and determining signal intensities corresponding to aperture ranges of different sizes by taking the mass center of the point source region as a center; noise variances corresponding to aperture ranges of different sizes are obtained based on the pixel gray value variances corresponding to the point source background areas; determining a target signal-to-noise ratio according to the signal intensity and the noise variance corresponding to each aperture range, and determining a target signal intensity and a target noise variance by using the target signal-to-noise ratio; and determining the maximum numerical magnitude actually observable by the astronomical telescope based on the target signal intensity and the target noise variance, and evaluating the imaging detection capability of the astronomical telescope on the celestial body according to the maximum numerical magnitude.

Description

TECHNICAL FIELD

[0001] The present application relates to the field of ground testing of space optical systems, and in particular to an astronomical telescope imaging detection capability evaluation method, device, equipment and medium. BACKGROUND

[0002] In the field of large space optical systems, astronomical telescopes are the core equipment for exploring the universe, and the accurate testing of their performance indicators directly determines the success or failure of the mission. Due to the high cost of astronomical telescopes and the difficulty of maintaining them after launch, comprehensive and strict performance verification needs to be completed during the ground integration testing phase, and the deep imaging observation magnitude is one of the core indicators, which directly reflects the detection capability of the telescope for extremely faint celestial bodies in the universe and is a key basis for evaluating the observation efficiency of the telescope.

[0003] However, there is a core technical problem in ground testing: the target observation magnitude of the telescope, such as 26th magnitude, corresponds to extremely low brightness of celestial bodies. Due to the influence of factors such as ground environmental light interference and light source simulation technology limitations, it is impossible to directly reproduce the light source of this brightness in the laboratory. To solve this problem, the existing technology generally adopts the testing idea of "high-brightness light source replacement", that is, by simulating a higher brightness magnitude for imaging, and then using data processing methods to extrapolate the actual observable target magnitude of the telescope.

[0004] Although this method avoids the difficulty of directly simulating the extremely faint target observation magnitude, its accuracy completely depends on the effectiveness of the data processing algorithm. The data processing method in the existing technology has obvious deficiencies in key links such as signal-to-noise ratio calculation, noise separation, and magnitude extrapolation. Especially when dealing with low signal-to-noise ratio images, it is difficult to accurately distinguish between signal and noise, resulting in a large error in the final calculated observation magnitude. SUMMARY

[0005] Therefore, the purpose of the present application is to provide an astronomical telescope imaging detection capability evaluation method, device, equipment and medium, which can accurately extrapolate the actual observation magnitude of the astronomical telescope through integrated data processing of point source image block extraction, multi-frame superposition, signal and noise separation calculation, maximum signal-to-noise ratio aperture optimization and magnitude extrapolation, and provide reliable technical support for the evaluation of the imaging detection capability of the telescope. The specific scheme is as follows:

[0006] In a first aspect, the present application provides an astronomical telescope imaging detection capability evaluation method, comprising:

[0007] Obtaining each point source image block based on a simulated light source, and superimposing each point source image block to obtain a target point source image block with the point source image peak value of the point source image block as the center; the point source image peak value is the maximum value of the signal intensity in the pixel region corresponding to the point source imaging;

[0008] splitting the target point source image block into a point source region and a point source background region, determining signal intensities corresponding to different sizes of aperture ranges respectively with the centroid of the point source region as the center;

[0009] determining a pixel gray value variance corresponding to the point source background region, and obtaining noise variances corresponding to the different sizes of aperture ranges respectively based on the pixel gray value variance;

[0010] determining a target signal-to-noise ratio with the largest signal-to-noise ratio according to the signal intensities and the noise variances corresponding to the different sizes of aperture ranges, and determining a target signal intensity and a target noise variance by using the target signal-to-noise ratio;

[0011] determining a maximum numerical stellar magnitude that can be actually observed by an astronomical telescope based on the target signal intensity and the target noise variance, and evaluating imaging and detection capabilities of the astronomical telescope on a target celestial body according to the maximum numerical stellar magnitude.

[0012] Optionally, the acquiring each point source image block based on the simulated light source comprises:

[0013] acquiring each frame of point source image based on the simulated light source;

[0014] for any frame of point source image, determining a background mean value corresponding to the any frame of point source image, extracting a point source image block from the any frame of point source image, and subtracting the background mean value from the point source image block to obtain each point source image block after preprocessing corresponding to each frame of point source image.

[0015] Optionally, the determining signal intensities corresponding to different sizes of aperture ranges respectively with the centroid of the point source region as the center comprises:

[0016] determining target apertures corresponding to different sizes of ratios respectively with the centroid of the point source region as the center and based on a ratio of a flow rate within an aperture to a total flow rate of the point source region;

[0017] for any target aperture, determining a flow sum of all pixels within the any target aperture, and determining the flow sum of the all pixels as a signal intensity corresponding to the any target aperture to obtain signal intensities corresponding to the target apertures respectively.

[0018] Optionally, the obtaining noise variances corresponding to the different sizes of aperture ranges respectively based on the pixel gray value variance comprises:

[0019] determining pixel numbers corresponding to each target aperture based on a focal length of a telescope system and a size of a pixel element corresponding to a detector; wherein the detector is located in the telescope system;

[0020] For any target aperture, the product of the pixel gray value variance and the pixel number corresponding to the target aperture is taken as the noise variance, to obtain the noise variance corresponding to the target aperture respectively.

[0021] Optionally, the target signal-to-noise ratio is determined according to the signal intensity and the noise variance corresponding to the different sizes of the aperture range, the target signal intensity and the target noise variance are determined by using the target signal-to-noise ratio, and the target signal intensity and the target noise variance are determined by using the target signal-to-noise ratio.

[0022] The signal-to-noise ratios corresponding to the different sizes of the aperture range are determined according to the signal intensity and the noise variance corresponding to the different sizes of the aperture range, and the maximum signal-to-noise ratio is determined as the target signal-to-noise ratio.

[0023] The target aperture range corresponding to the target signal-to-noise ratio is determined, and the signal intensity and the noise variance corresponding to the target aperture range are taken as the target signal intensity and the target noise variance.

[0024] Optionally, the maximum numerical star magnitude that can be actually observed by the astronomical telescope is determined based on the target signal intensity and the target noise variance, and the maximum numerical star magnitude that can be actually observed by the astronomical telescope is determined based on the target signal intensity and the target noise variance.

[0025] The target coefficient is determined based on the target signal intensity, the target noise variance and a preset signal-to-noise ratio.

[0026] The actual star magnitude corresponding to the simulated light source is determined, and the maximum numerical star magnitude that can be actually observed by the astronomical telescope is determined according to the target coefficient and the actual star magnitude.

[0027] Optionally, the target coefficient is determined based on the target signal intensity, the target noise variance and a preset signal-to-noise ratio.

[0028] The target coefficient is determined based on the target signal intensity, the target noise variance, a preset signal-to-noise ratio and a preset target equation.

[0029] The target equation is:

[0030] ;

[0031] Wherein, k is the target coefficient, is the target signal intensity, M is a preset signal-to-noise ratio, is the target noise variance; wherein, is the number of pixels in the aperture range corresponding to the target signal-to-noise ratio, is the pixel gray value variance corresponding to the point source background region.

[0032] In a second aspect, the present application provides an astronomical telescope imaging detection capability evaluation device, comprising:

[0033] An image block acquisition module is configured to acquire each point source image block obtained based on the simulated light source, and to superimpose each point source image block to obtain a target point source image block, with a point source image peak value of the point source image block as a center; the point source image peak value is a maximum value of signal intensity in a pixel region corresponding to point source imaging;

[0034] A signal intensity determination module is configured to split the target point source image block into a point source region and a point source background region, and to determine signal intensity corresponding to different aperture ranges of different sizes with a center of mass of the point source region as a center;

[0035] A noise variance determination module is configured to determine a pixel gray value variance corresponding to the point source background region, and to obtain noise variance corresponding to the different aperture ranges of different sizes based on the pixel gray value variance;

[0036] A target data determination module is configured to determine a target signal-to-noise ratio with the maximum signal-to-noise ratio according to the signal intensity and the noise variance corresponding to the different aperture ranges of different sizes, and to determine a target signal intensity and a target noise variance by using the target signal-to-noise ratio;

[0037] A star magnitude determination module is configured to determine a maximum numerical star magnitude that can be observed by an astronomical telescope based on the target signal intensity and the target noise variance, and to evaluate imaging and detection capability of the astronomical telescope on a target celestial body according to the maximum numerical star magnitude.

[0038] In a third aspect, the present application provides an electronic device, comprising:

[0039] A memory is configured to save a computer program;

[0040] A processor is configured to execute the computer program to implement the aforementioned astronomical telescope imaging and detection capability evaluation method.

[0041] In a fourth aspect, the present application provides a computer readable storage medium configured to save a computer program, wherein the computer program is executed by a processor to implement the aforementioned astronomical telescope imaging and detection capability evaluation method.

[0042] In the present application, each point source image block obtained based on the simulated light source is superimposed to obtain a target point source image block, with the point source image peak of the point source image block as the center. The point source image peak is the maximum value of signal intensity in the corresponding pixel region after point source imaging. The target point source image block is split into a point source region and a point source background region, and the signal intensity corresponding to different aperture ranges is determined with the center of mass of the point source region as the center. The pixel gray value variance corresponding to the point source background region is determined, and the noise variance corresponding to the different aperture ranges is obtained based on the pixel gray value variance. The target signal-to-noise ratio with the maximum signal-to-noise ratio is determined according to the signal intensity and noise variance corresponding to the different aperture ranges, and the target signal intensity and target noise variance are determined using the target signal-to-noise ratio. The maximum numerical magnitude of the star magnitude that can be actually observed by the astronomical telescope is determined based on the target signal intensity and the target noise variance, and the imaging detection capability of the astronomical telescope for the target celestial body is evaluated according to the maximum numerical magnitude of the star magnitude. As can be seen from the above, the present application superimposes each point source image block with the center of the point source image peak, so that the point source signal is accumulated and enhanced in the superposition, and the randomly distributed noise is offset, thereby improving the recognizability of low brightness signal from the source, laying a foundation for subsequent accurate calculation, and avoiding the technical bottleneck of directly simulating extremely dark star magnitude. The target point source image block after superposition is explicitly split into a point source region and a point source background region, and the pixel gray value variance of the background region is calculated separately to represent the noise intensity, thereby avoiding the error caused by mixed calculation of signal and noise in the prior art, and ensuring the accuracy of the noise variance data. The center of mass of the point source region is set as the center, different aperture ranges are set, and the corresponding signal intensity is calculated, combined with the noise variance of the background region, and the signal-to-noise ratio of each aperture is calculated one by one, and finally the target aperture with the maximum signal-to-noise ratio and the corresponding signal and noise data are selected. This design fully adapts to the point source flow distribution characteristics, ensures the acquisition of the most accurate target signal-to-noise ratio, and solves the problem of difficult distinction between signal and noise in low signal-to-noise ratio images. Finally, based on the accurate target signal intensity and target noise variance, the star magnitude is extrapolated. Since the previous steps have realized the accurate separation of signal and noise and the optimized selection of signal-to-noise ratio, the star magnitude extrapolation provides reliable basic data. Compared with the inaccurate data in the prior art affected by noise, the finally calculated maximum observation star magnitude of the astronomical telescope is closer to the actual performance, and the star magnitude calculation error is greatly reduced. BRIEF DESCRIPTION OF DRAWINGS

[0043] In order to more clearly illustrate the technical solutions in the embodiments of the present application or the prior art, the following will briefly introduce the drawings needed to be used in the embodiments or prior art description. Obviously, the drawings in the following description are only embodiments of the present application, and those skilled in the art can also obtain other drawings according to the provided drawings without creating any inventive labor.

[0044] Figure 1 A flow chart of an astronomical telescope imaging detection capability evaluation method disclosed in the present application;

[0045] Figure 2 A schematic diagram of a data processing process disclosed in the present application;

[0046] Figure 3 A flow chart of a specific astronomical telescope imaging detection capability evaluation method disclosed in the present application;

[0047] Figure 4 A schematic diagram of an astronomical telescope imaging detection capability evaluation device structure disclosed in the present application;

[0048] Figure 5 A schematic diagram of an electronic device structure disclosed in the present application. DETAILED DESCRIPTION

[0049] The technical solutions in the embodiments of the present application will be clearly and completely described below with reference to the drawings in the embodiments of the present application. Obviously, the described embodiments are only part of the embodiments of the present application, not all the embodiments. Based on the embodiments in the present application, all other embodiments obtained by those skilled in the art without creative labor are within the scope of protection of the present application.

[0050] Nowadays, a core technical problem is faced in ground testing: the target observation star magnitude of the telescope corresponds to extremely low brightness of celestial bodies. Influenced by factors such as ground environmental light interference and light source simulation technology limitation, the light source of this brightness cannot be directly reproduced in the laboratory. The data processing method in the prior art has obvious deficiencies in key links such as signal-to-noise ratio calculation, noise separation and star magnitude extrapolation, especially when processing low signal-to-noise ratio images, it is difficult to accurately distinguish signal and noise, resulting in large errors in the final calculated observation star magnitude. Therefore, the present application provides an astronomical telescope imaging detection capability evaluation method, which can accurately extrapolate the actual observation star magnitude of the astronomical telescope through integrated data processing of point source image block extraction, multi-frame superposition, signal and noise separation calculation, maximum signal-to-noise ratio aperture optimization and star magnitude extrapolation, and provides reliable technical support for the imaging detection capability evaluation of the telescope.

[0051] Referring to Figure 1 The embodiments of the present application disclose an astronomical telescope imaging detection capability evaluation method, which comprises:

[0052] Step S11, obtaining each point source image block obtained based on the simulated light source, and superimposing each point source image block to obtain a target point source image block with the point source image peak value of the point source image block as the center; the point source image peak value is the maximum value of the signal intensity in the pixel region corresponding to the point source imaging.

[0053] In this embodiment, first, 2N 2N point source image blocks can be extracted from each frame containing point source images, specifically, each frame point source image corresponding background mean value can be determined, and point source image blocks can be extracted from each frame point source image, and the background mean value can be subtracted from the point source image blocks to obtain each frame point source image corresponding to each point source image block after preprocessing. The point source image block contains a background area, but the background mean value has been subtracted as a whole, that is, the background part mean value is zero.

[0054] Then, the point source image peak of the point source image block is taken as the center, and each point source image block is superimposed, as shown in Figure 2 The superimposed target point source image block is obtained, and since each point source image block is centered on the point source image peak, the superimposing process actually includes an image registration process.

[0055] Step S12, the target point source image block is split into a point source region and a point source background region, and the signal intensity corresponding to the aperture range of different sizes is determined with the centroid of the point source region as the center.

[0056] In this embodiment, the superimposed target point source image block is split into N N size point source region and surrounding point source background region, as shown in Figure 2 The point source region is used to calculate the point source flow, that is, the signal intensity, and the point source background region is used to calculate the noise intensity.

[0057] Specifically, the centroid of the point source region can be taken as the center, and based on the ratio of the flow within the aperture to the total flow of the point source region, the target aperture corresponding to the ratio of different sizes can be determined, as shown in Figure 2 R_EE50, R_EE60, R_EE70, R_EE80, R_EE90. For any target aperture, the flow sum of all pixels within any target aperture is determined, and the flow sum of all pixels is determined as the signal intensity corresponding to any target aperture, to obtain the signal intensity corresponding to the target aperture of different sizes. For example, the flow within the aperture accounts for 80% of the total flow of the point source region, and a aperture size can be determined, and different proportions can correspond to different aperture sizes.

[0058] Step S13, determine the pixel gray value variance corresponding to the point source background region, and obtain the noise variance corresponding to the aperture range of different sizes based on the pixel gray value variance.

[0059] Further, the pixel gray value variance corresponding to the point source background region can be determined, and then the number of pixels corresponding to each target aperture can be determined based on the focal length of the telescope system and the size of the pixel corresponding to the detector. The detector is located in the telescope system. For any target aperture, the product of the pixel gray value variance and the number of pixels corresponding to any target aperture is taken as the noise variance to obtain the noise variance corresponding to each target aperture.

[0060] In step S14, the target signal-to-noise ratio with the maximum signal-to-noise ratio is determined according to the signal intensity and the noise variance corresponding to the aperture range of different sizes, and the target signal intensity and the target noise variance are determined using the target signal-to-noise ratio.

[0061] After obtaining the signal intensity and the noise variance corresponding to the aperture range of different sizes, the signal-to-noise ratio corresponding to the aperture range of different sizes can be determined according to the signal intensity and the noise variance corresponding to the aperture range of different sizes, and the maximum signal-to-noise ratio is determined as the target signal-to-noise ratio. The target aperture range corresponding to the target signal-to-noise ratio is determined, and the signal intensity and the noise variance corresponding to the target aperture range are taken as the target signal intensity and the target noise variance.

[0062] The signal-to-noise ratio calculation formula is as follows:

[0063] ;

[0064] S is the signal intensity, is the pixel gray value variance corresponding to the point source background region, is the noise variance, is the noise intensity.

[0065] In step S15, the maximum numerical magnitude of the star magnitude that can be actually observed by the astronomical telescope is determined based on the target signal intensity and the target noise variance, so as to evaluate the imaging and detection capability of the astronomical telescope on the target celestial body according to the maximum numerical magnitude of the star magnitude.

[0066] In this embodiment, first, the target coefficient can be determined based on the target signal intensity, the target noise variance, and the preset signal-to-noise ratio. Then, the actual star magnitude corresponding to the simulated light source can be determined, and the maximum numerical magnitude of the star magnitude that can be actually observed by the astronomical telescope is determined according to the target coefficient and the actual star magnitude.

[0067] The target coefficient can be determined based on the target signal intensity, the target noise variance, and the preset signal-to-noise ratio, which can include determining the target coefficient based on the target signal intensity, the target noise variance, the preset signal-to-noise ratio, and a preset target equation. The target equation is:

[0068] ;

[0069] wherein k is the target coefficient, M is a preset signal-to-noise ratio, is a target noise variance; wherein, is the number of pixels in the aperture range corresponding to the target signal-to-noise ratio, is the pixel gray value variance corresponding to the point source background area.

[0070] Taking M as 5, we can get:

[0071] ;

[0072] k needs to take a positive value, and the maximum value of the star magnitude that can be observed under the actual exposure time is:

[0073] ;

[0074] wherein, is the star magnitude simulated by the light source, if is 25.5 magnitude, and needs Under the condition, the signal-to-noise ratio can reach 5, and the actual observation star magnitude of the optical facility is , that is, only 24.5 magnitude can be observed.

[0075] As can be seen from the above and as shown in Figure 3 , the embodiment can accurately extrapolate the actual observation star magnitude of the astronomical telescope through the processes of point source image block extraction, point source image block superposition, split of the superposed point source image block, signal intensity calculation, noise intensity calculation, signal-to-noise ratio calculation in different apertures, maximum signal-to-noise ratio aperture size determination, and star magnitude extrapolation, solves the technical bottleneck that the low brightness target star magnitude cannot be directly simulated on the ground, and provides reliable technical support for the imaging detection capability evaluation of the telescope.

[0076] Referring to Figure 4 , the embodiment of the application further discloses an astronomical telescope imaging detection capability evaluation device, which comprises:

[0077] An image block acquisition module 11 is configured to acquire each point source image block obtained based on a simulated light source, and to superpose each point source image block to obtain a target point source image block, with a point source image peak value of the point source image block as the center; the point source image peak value is the maximum value of the signal intensity in the pixel area corresponding to the point source imaging;

[0078] A signal intensity determination module 12 is configured to split the target point source image block into a point source area and a point source background area, and to determine the signal intensity corresponding to different sizes of aperture ranges with the centroid of the point source area as the center;

[0079] The noise variance determination module 13 is configured to determine a pixel gray value variance corresponding to the point source background region, and determine noise variances corresponding to the different sizes of the aperture ranges based on the pixel gray value variance.

[0080] The target data determination module 14 is configured to determine a target signal-to-noise ratio (SNR) with the maximum SNR according to the signal intensity and the noise variance corresponding to the different sizes of the aperture ranges, and determine a target signal intensity and a target noise variance by using the target SNR.

[0081] The star magnitude determination module 15 is configured to determine a maximum numerical star magnitude that can be observed by the astronomical telescope based on the target signal intensity and the target noise variance, and evaluate the imaging and detection capability of the astronomical telescope for a target celestial body according to the maximum numerical star magnitude.

[0082] In some embodiments, the image block acquisition module 11 comprises:

[0083] An image acquisition unit is configured to acquire each frame of point source image based on a simulated light source.

[0084] A preprocessing unit is configured to, for any frame of point source image, determine a background mean value corresponding to the any frame of point source image, extract a point source image block from the any frame of point source image, and subtract the background mean value from the point source image block to obtain each frame of point source image block after preprocessing.

[0085] In some embodiments, the signal intensity determination module 12 comprises:

[0086] An aperture determination unit is configured to determine target apertures corresponding to different sizes of a ratio based on the ratio of the flow within the aperture to the total flow of the point source region and with the centroid of the point source region as the center.

[0087] A signal intensity determination unit is configured to, for any target aperture, determine a flow sum of all pixels within the any target aperture, and determine the flow sum of the all pixels as a signal intensity corresponding to the any target aperture, so as to obtain the signal intensity corresponding to the target aperture.

[0088] In some embodiments, the noise variance determination module 13 comprises:

[0089] A pixel number determination unit is configured to determine a pixel number corresponding to each target aperture based on a focal length of a telescope system and a pixel size corresponding to a detector, wherein the detector is located in the telescope system.

[0090] a noise variance determination unit configured to determine, for any target aperture, a product of the pixel gray value variance and a pixel number corresponding to the target aperture as a noise variance corresponding to the target aperture, to obtain a noise variance corresponding to each target aperture.

[0091] In some embodiments, the target data determination module 14 comprises:

[0092] a signal-to-noise ratio (SNR) calculation unit configured to determine, according to the signal intensity and the noise variance corresponding to each aperture range, an SNR corresponding to each aperture range, and determine a maximum SNR as a target SNR;

[0093] a data determination unit configured to determine a target aperture range corresponding to the target SNR, and determine a signal intensity and a noise variance corresponding to the target aperture range as a target signal intensity and a target noise variance.

[0094] In some embodiments, the star magnitude determination module 15 comprises:

[0095] a coefficient determination sub-module configured to determine a target coefficient based on the target signal intensity, the target noise variance, and a preset SNR;

[0096] a star magnitude determination unit configured to determine an actual star magnitude corresponding to the simulated light source, and determine a maximum numerical star magnitude that can be observed by the astronomical telescope according to the target coefficient and the actual star magnitude.

[0097] In some embodiments, the coefficient determination sub-module comprises:

[0098] a coefficient determination unit configured to determine a target coefficient based on the target signal intensity, the target noise variance, a preset SNR, and a preset target equation;

[0099] The target equation is:

[0100] ;

[0101] wherein k is the target coefficient, is the target signal intensity, M is the preset SNR, is the target noise variance; wherein, is a pixel number in an aperture range corresponding to the target SNR, is a pixel gray value variance corresponding to a point source background region.

[0102] Further, the embodiments of the present application also disclose an electronic device, Figure 5 is a structural diagram of an electronic device 20 according to an exemplary embodiment, and the contents in the diagram cannot be considered as any limitation on the use range of the present application.

[0103] Figure 5 A structural schematic diagram of an electronic device 20 is provided in the embodiment. The electronic device 20 can specifically include at least one processor 21, at least one memory 22, a power supply 23, a communication interface 24, an input / output interface 25 and a communication bus 26. The memory 22 is configured to store a computer program, and the processor 21 is configured to load and execute the computer program to implement the related steps in the astronomical telescope imaging detection capability evaluation method disclosed in any of the foregoing embodiments. In addition, the electronic device 20 in the embodiment can be specifically an electronic computer.

[0104] In the embodiment, the power supply 23 is configured to provide working voltage for each hardware device on the electronic device 20; the communication interface 24 is configured to create a data transmission channel between the electronic device 20 and external devices, and the communication protocol followed by the communication interface 24 can be any communication protocol applicable to the technical solution of the present application, which is not specifically limited here; the input / output interface 25 is configured to obtain external input data or output data to the outside, and the specific interface type can be selected according to the specific application needs, which is not specifically limited here.

[0105] In addition, the memory 22 as a carrier for resource storage can be a read-only memory, a random access memory, a magnetic disk or an optical disk, etc., and the resources stored thereon can include an operating system 221, a computer program 222, etc., and the storage mode can be temporary storage or permanent storage.

[0106] The operating system 221 is configured to manage and control each hardware device on the electronic device 20 and the computer program 222, and can be Windows Server, Netware, Unix, Linux, etc. In addition to the computer program capable of completing the astronomical telescope imaging detection capability evaluation method executed by the electronic device 20 disclosed in any of the foregoing embodiments, the computer program 222 can further include a computer program capable of completing other specific work.

[0107] Further, the present application further discloses a computer readable storage medium for storing a computer program; wherein the computer program is executed by a processor to implement the astronomical telescope imaging detection capability evaluation method disclosed above. For the specific steps of the method, reference can be made to the corresponding content disclosed in the foregoing embodiments, which will not be repeated here.

[0108] The various embodiments described in the specification are progressive in nature, and each embodiment highlights the differences from other embodiments. The same or similar parts among the various embodiments can be mutually referred to. For the apparatus disclosed by the embodiments, since it corresponds to the method disclosed by the embodiments, the description is relatively simple, and the relevant parts can be referred to the method part.

[0109] Those skilled in the art will further appreciate that the individual steps of the examples described in connection with the embodiments disclosed herein can be embodied in electronic hardware, computer software, or combinations of both. The various examples have been described in relation to the described embodiments, as a means of generalizing the interchangeability of hardware and software under the principles mentioned above. The particular implementation of an individual example in either hardware or software can be determined by the particular application and design constraints imposed on the overall system. Skilled artisans will appreciate that the principles described herein can be practiced in a variety of system environments, and that the described implementations are merely examples and not intended to limit the scope of the application.

[0110] The steps of a method or algorithm described in connection with the embodiments disclosed herein can be embodied directly in hardware, in a software module executed by a processor, or in a combination of the two. A software module can reside in random access memory (RAM), flash memory, read-only memory (ROM), electrically programmable ROM (EPROM), electrically erasable programmable ROM (EEPROM), registers, hard disk, a removable disk, a CD-ROM, or any other form of storage medium known in the art.

[0111] Finally, it needs to be pointed out that, in this document, the relationship terms such as first and second are only used to distinguish one entity or operation from another entity or operation, and do not necessarily require or imply any such actual relationship or order between the entities or operations. Moreover, the terms "include", "contain" or any other variants thereof are intended to cover non-exclusive inclusion, so that the process, method, article or device including a series of elements not only includes those elements, but also includes other elements not explicitly listed or inherent to such process, method, article or device. Without more limitations, the element defined by the statement "including a" does not exclude the presence of other identical elements in the process, method, article or device including the element.

[0112] The above describes the technical solutions provided by the present application in detail, and the principles and implementation manners of the present application are described by using specific examples. The above description of the embodiments is only for helping to understand the method and core idea of the present application; at the same time, for those skilled in the art, according to the idea of the present application, the specific implementation manner and application range can be changed, and the above description of the specification should not be understood as limiting the present application.

Claims

1. A method for evaluating the imaging and detection capabilities of an astronomical telescope, characterized in that, include: Obtain each point source image block based on the simulated light source, and superimpose each point source image block with the point source image peak value of the point source image block as the center to obtain the target point source image block; The peak value of the point source image is the maximum signal intensity in the corresponding pixel region after the point source is imaged; The target point source image block is divided into a point source region and a point source background region. The signal intensity corresponding to different aperture ranges is determined with the centroid of the point source region as the center. Determine the pixel grayscale value variance corresponding to the point source background region, and obtain the noise variance corresponding to the different aperture ranges based on the pixel grayscale value variance; The target signal-to-noise ratio with the largest signal-to-noise ratio is determined based on the signal strength and noise variance corresponding to the different aperture ranges, and the target signal strength and target noise variance are determined using the target signal-to-noise ratio; The maximum magnitude that the astronomical telescope can actually observe is determined based on the target signal strength and the target noise variance, so as to evaluate the astronomical telescope's imaging and detection capability of the target celestial body based on the maximum magnitude.

2. The method for evaluating the imaging and detection capabilities of astronomical telescopes according to claim 1, characterized in that, The acquisition of point source image patches based on simulated light sources includes: Acquire point source images for each frame based on simulated light sources; For any frame of point source image, determine the background mean value corresponding to the frame of point source image, extract point source image blocks from the frame of point source image, and subtract the background mean value from the point source image blocks to obtain the preprocessed point source image blocks corresponding to each frame of point source image.

3. The method for evaluating the imaging and detection capabilities of astronomical telescopes according to claim 1, characterized in that, The step of determining the signal intensity corresponding to different aperture ranges centered on the centroid of the point source region includes: Centered on the centroid of the point source region, and based on the ratio of the flow rate within the orifice to the total flow rate of the point source region, the target orifice diameters corresponding to different ratios are determined. For any target aperture, the sum of flux of all pixels within the target aperture is determined, and the sum of flux of all pixels is determined as the signal strength corresponding to the target aperture, so as to obtain the signal strength corresponding to the target aperture respectively.

4. The method for evaluating the imaging and detection capabilities of astronomical telescopes according to claim 3, characterized in that, The step of obtaining the noise variance corresponding to the different aperture ranges based on the pixel grayscale value variance includes: The number of pixels corresponding to each target aperture is determined based on the focal length of the telescope system and the pixel size corresponding to the detector; wherein, the detector is located in the telescope system; For any target aperture, the product of the pixel grayscale value variance and the number of pixels corresponding to any target aperture is used as the noise variance to obtain the noise variance corresponding to each target aperture.

5. The method for evaluating the imaging and detection capabilities of astronomical telescopes according to claim 1, characterized in that, The step of determining the target signal-to-noise ratio (SNR) with the largest SNR based on the signal strength and noise variance corresponding to the different aperture ranges, and using the target SNR to determine the target signal strength and target noise variance, includes: The signal-to-noise ratios corresponding to the different aperture ranges are determined based on the signal strength and noise variance corresponding to the different aperture ranges, and the maximum signal-to-noise ratio is determined as the target signal-to-noise ratio. Determine the target aperture range corresponding to the target signal-to-noise ratio, and use the signal strength and noise variance corresponding to the target aperture range as the target signal strength and target noise variance.

6. The method for evaluating the imaging and detection capabilities of astronomical telescopes according to claim 5, characterized in that, The determination of the maximum magnitude that the astronomical telescope can actually observe based on the target signal strength and the target noise variance includes: The target coefficients are determined based on the target signal strength, the target noise variance, and the preset signal-to-noise ratio. Determine the actual magnitude corresponding to the simulated light source, and determine the maximum magnitude that the astronomical telescope can actually observe based on the target coefficient and the actual magnitude.

7. The method for evaluating the imaging and detection capabilities of astronomical telescopes according to claim 6, characterized in that, The step of determining the target coefficient based on the target signal strength, the target noise variance, and a preset signal-to-noise ratio includes: The target coefficients are determined based on the target signal strength, the target noise variance, the preset signal-to-noise ratio, and the preset target equation. The objective equation is: ； Where k is the target coefficient. The target signal strength is M, and the preset signal-to-noise ratio is M. Let be the target noise variance; where, The number of pixels within the aperture range corresponding to the target signal-to-noise ratio. This represents the variance of the pixel grayscale values ​​corresponding to the point source background region.

8. A device for evaluating the imaging and detection capabilities of an astronomical telescope, characterized in that, include: The image block acquisition module is used to acquire each point source image block based on the simulated light source, and to superimpose each point source image block with the point source image peak value of the point source image block as the center to obtain the target point source image block. The peak value of the point source image is the maximum signal intensity in the corresponding pixel region after the point source is imaged; The signal strength determination module is used to divide the target point source image block into a point source region and a point source background region, and determine the signal strength corresponding to different aperture ranges with the centroid of the point source region as the center. The noise variance determination module is used to determine the pixel gray value variance corresponding to the point source background region, and obtain the noise variance corresponding to the different aperture ranges based on the pixel gray value variance; The target data determination module is used to determine the target signal-to-noise ratio with the largest signal-to-noise ratio based on the signal strength and noise variance corresponding to the different aperture ranges, and to determine the target signal strength and target noise variance using the target signal-to-noise ratio; The magnitude determination module is used to determine the maximum magnitude that the astronomical telescope can actually observe based on the target signal strength and the target noise variance, so as to evaluate the imaging and detection capability of the astronomical telescope for the target celestial body based on the maximum magnitude.

9. An electronic device, characterized in that, include: Memory, used to store computer programs; A processor for executing the computer program to implement the method for evaluating the imaging and detection capabilities of astronomical telescopes as described in any one of claims 1 to 7.

10. A computer-readable storage medium, characterized in that, Used to store a computer program, which, when executed by a processor, implements the method for evaluating the imaging and detection capabilities of an astronomical telescope as described in any one of claims 1 to 7.

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