Adjustment method and device for improving imaging resolution of telescope system

Abstract

The invention relates to an adjusting method and device for improving the imaging resolution of a large-aperture telescope system, and the method comprises the steps: obtaining a dynamic surface type of the telescope system through an acceleration sensor, carrying out the optical inversion through the combination of the dynamic surface type and the propagation law of Fourier optics, and constructing an instantaneous point spread function of the system, and image deconvolution is carried out based on the point spread function so as to obtain an imaging effect with a higher resolution.

Description

Technical Field

[0001] This invention relates to the field of telescope optics, and more specifically, to a method and apparatus for adjusting the imaging resolution of a telescope system. Background Technology

[0002] The imaging process of large-aperture optical elements can be approximated as the convolution of the object's light field information and the point spread function. Common optical systems use Airy disks as the convolution kernel, while the kernel of a large-aperture stitching system is determined by the state of the optical system. Large-aperture, wide-field-of-view telescopes employ a convolutional kernel system, utilizing an all-optical image convolution system with a spatial light modulator as the primary mirror. Combined with pixel merging, a simple convolutional neural network is used to perform optical calculations on gravitational lensing; the output is the solution result, requiring no further processing.

[0003] Current large-aperture, wide-field-of-view telescope systems suffer from poor image resolution due to external interference causing a decline in system alignment and imaging quality, as well as the impact of telescope system jitter on the final image contrast. Therefore, existing technologies still have shortcomings and require further development. Summary of the Invention

[0004] This invention provides a method and apparatus for improving the imaging resolution of a large-aperture telescope system, thereby at least solving the technical problem of low image resolution in existing large-aperture telescope systems.

[0005] According to an embodiment of the present invention, a method for improving the imaging resolution of a large-aperture telescope system is provided, comprising the following steps: At least three accelerometers are placed after each sub-mirror in the segmented splicing telescope system; The initial position of each sub-mirror is accurately measured using a spatial coordinate measuring device, and the spatial three-dimensional position of all sub-mirrors is measured at high frequency based on the position of each sub-mirror and the calibrated sensitive axis direction. By using accelerometers on each splicing sub-mirror, a real-time overall mirror surface shape representation is constructed. Based on the constructed overall mirror surface shape representation combined with the working wavelength, a new surface shape measurement system that does not require direct imaging and exposure integration is constructed. Based on a new surface shape measurement system, the dynamic surface shape of the telescope system obtained by the accelerometer is combined with the propagation law of Fourier optics to perform optical inversion, construct the instantaneous point spread function of the telescope system, and perform image deconvolution using the point spread function to obtain higher resolution imaging effect.

[0006] Furthermore, the initial position of each sub-mirror is precisely measured using a spatial coordinate measuring device, specifically as follows: The initial position of each sub-mirror is precisely measured using a coordinate measuring machine.

[0007] Furthermore, the method also includes: The spatial positions of the primary mirror, secondary mirror, and final mirror of the telescope system are measured using laser ranging.

[0008] Furthermore, after accurately measuring the initial position of each sub-mirror using a spatial coordinate measuring device, and performing high-frequency measurements of the three-dimensional spatial positions of all sub-mirrors based on the position of each sub-mirror and the calibrated sensitive axis direction, the method further includes: The pose of each sub-mirror is measured, and the real-time feedback of the pose measurement results reduces the jitter of the telescope system and its impact on the final image contrast.

[0009] Furthermore, each sub-mirror retains six degrees of freedom.

[0010] Furthermore, the expression for the point spread function is:

[0011] in The dynamic point spread function characterizes stability. Let t be the integration time, and t be the diffusion function at that time point.

[0012] Furthermore, performing a Fourier transform on the point spread function yields the transformed expression:

[0013] Modulation transfer function characterizing dynamic stability ,in For spatial frequency, For the integration time, the first The setting of each link The overall formula is as follows, which can be used to characterize high-frequency stability:

[0014] Where N is the total number of system components, the relationship between mechanical resonance, system control and optics can be established by using the dynamic transfer function based on the static evaluation of the optical system; ultimately, the effective characterization of multi-temporal boundary interaction effects in the spatiotemporal frequency domain can be achieved.

[0015] A method for adjusting the imaging resolution of a telescope system, comprising: The mounting module is used to place at least three accelerometers after each sub-mirror in a segmented splicing telescope system. The measurement module is used to accurately measure the initial position of each sub-mirror using a spatial coordinate measuring device, and to perform high-frequency measurements of the three-dimensional spatial position of all sub-mirrors based on the position of each sub-mirror and the calibrated sensitive axis direction. The system construction module is used to construct a real-time overall mirror surface shape expression through the accelerometer on each splicing sub-mirror, and based on the constructed overall mirror surface shape expression combined with the working wavelength, to construct a new surface shape measurement system that does not require direct imaging and exposure integration; The image processing module is used to obtain the dynamic surface profile of the telescope system through the accelerometer based on the new surface profile measurement system. It combines the dynamic surface profile with the propagation law of Fourier optics to perform optical inversion, construct the instantaneous point spread function of the telescope system, and perform image deconvolution using the point spread function to obtain higher resolution imaging effect.

[0016] A computer-readable medium, a computer-readable storage medium storing one or more programs, which can be executed by one or more processors to implement the steps in the adjustment method for improving imaging resolution of a telescope system as described in any of the preceding claims.

[0017] A terminal device includes: a processor, a memory, and a communication bus; the memory stores a computer-readable program that can be executed by the processor; The communication bus enables communication between the processor and memory; When the processor executes a computer-readable program, it implements the steps in the adjustment method for improving the imaging resolution of the telescope system as described above.

[0018] The present invention relates to a method and apparatus for improving the imaging resolution of a large-aperture telescope system. This application obtains the dynamic surface profile of the telescope system from an accelerometer, combines the dynamic surface profile with the propagation laws of Fourier optics to perform optical inversion, constructs the instantaneous point spread function of the system, and uses this point spread function to perform image deconvolution to obtain a higher resolution imaging effect. Attached Figure Description

[0019] The accompanying drawings, which are included to provide a further understanding of the invention and form part of this application, illustrate exemplary embodiments of the invention and, together with their description, serve to explain the invention and do not constitute an undue limitation thereof. In the drawings: Figure 1 This is a flowchart of the method for adjusting the imaging resolution of the large-aperture telescope system of the present invention; Figures 2-10 This is a diagram showing the wavefront and corresponding image of the digital adaptive optics of this invention; Figure 11 This is a block diagram of the adjustment device for improving imaging resolution in the large-aperture telescope system of the present invention; Figure 12 This is a diagram of the terminal device of the present invention; Figures 13-14 This is a schematic diagram of the passive damping of the present invention. Detailed Implementation

[0020] To enable those skilled in the art to better understand the present invention, the technical solutions of the present invention will be clearly and completely described below with reference to the accompanying drawings of the embodiments of the present invention. Obviously, the described embodiments are only some embodiments of the present invention, and not all embodiments. Based on the embodiments of the present invention, all other embodiments obtained by those skilled in the art without creative effort should fall within the scope of protection of the present invention.

[0021] It should be noted that the terms "first," "second," etc., in the specification, claims, and accompanying drawings of this invention are used to distinguish similar objects and are not necessarily used to describe a specific order or sequence. It should be understood that such data can be interchanged where appropriate so that the embodiments of the invention described herein can be implemented in orders other than those illustrated or described herein. Furthermore, the terms "comprising" and "having," and any variations thereof, are intended to cover a non-exclusive inclusion; for example, a process, method, system, product, or apparatus that comprises a series of steps or units is not necessarily limited to those steps or units explicitly listed, but may include other steps or units not explicitly listed or inherent to such processes, methods, products, or apparatus.

[0022] Example 1 According to an embodiment of the present invention, a method for improving the imaging resolution of a large-aperture telescope system is provided, see [link to relevant documentation]. Figure 1 This includes the following steps: S100: Place at least three accelerometers after each sub-mirror in a segmented splicing telescope system; S200: The initial position of each sub-mirror is accurately measured using a spatial coordinate measuring device, and the spatial three-dimensional position of all sub-mirrors is measured at high frequency based on the position of each sub-mirror and the calibrated sensitive axis direction. S300: By using the accelerometer on each splicing sub-mirror, a real-time overall mirror surface shape expression is constructed, and based on the constructed overall mirror surface shape expression combined with the working wavelength, a new surface shape measurement system is constructed that does not require direct imaging and exposure integration. S400: Based on a new surface shape measurement system, the dynamic surface shape of the telescope system is obtained through an accelerometer. The dynamic surface shape is combined with the propagation law of Fourier optics to perform optical inversion, construct the instantaneous point spread function of the telescope system, and perform image deconvolution using the point spread function to obtain higher resolution imaging effect.

[0023] This application uses the dynamic surface profile of the telescope system obtained by the accelerometer to perform optical inversion by combining the dynamic surface profile with the propagation law of Fourier optics, constructs the instantaneous point spread function of the system, and uses this point spread function to perform image deconvolution to obtain a higher resolution imaging effect.

[0024] The following describes the specific steps of the method for improving the imaging resolution of the large-aperture telescope system described in this application: Step 1: For segmented, modular telescopes, place at least three accelerometers after each sub-mirror to enable high-frequency measurements of their spatial position.

[0025] Step 2: Use a coordinate measuring machine or other spatial coordinate measuring equipment to measure its initial position with high precision, and based on its position and the calibrated sensitive axis direction, measure its three-dimensional position in space with high frequency.

[0026] Step 3: Using accelerometers on each splicing sub-diameter, construct a real-time overall mirror surface shape representation, and based on this representation combined with the working wavelength, construct a new surface shape measurement system that does not require direct imaging and exposure integration.

[0027] Step 4: Using the dynamic surface profile of the system obtained from the accelerometer, optical inversion is performed by combining it with the propagation laws of Fourier optics to construct the instantaneous point spread function of the system. This point spread function is then used for image deconvolution to obtain higher resolution imaging. Specifically, it includes: 1. Use laser rangefinder to measure the spatial position between the primary mirror, secondary mirror, and subsequent intermediate mirror to ensure the system's alignment and basic phase difference limits.

[0028] Second: First, for the laser ranging part in the optical truss, spatial kinematics is used to construct a more advanced three-dimensional position from low-level geometric elements. Through the interactive iteration of important positional quantities such as mutual rotation and eccentricity of components with the optical design model, the low-order errors of the system can be controlled.

[0029] Thirdly, to address the contradiction between integration time and sensitivity in system jitter measurement, an accelerometer is used to measure the pose of each sub-mirror. Through real-time feedback, the jitter of the system and its impact on the final image contrast are reduced.

[0030] Fourth: Active optics, as a key technology for large-aperture telescopes, has been widely applied. To further enhance the detection capabilities of large-aperture telescopes, active optics enables independent, real-time surface correction and attitude control of each major component. This not only reduces the requirements for optical processing and system assembly precision but also effectively relaxes the rigidity requirements of large tracking frames, reducing system inertia. Because large-aperture telescopes undertake more observation tasks, their mission schedules are more tightly scheduled, and longer observation times directly impact the results, leading to more challenging external observation environments.

[0031] Fifth: Since each sub-mirror has only six degrees of freedom, and the degree of freedom along the optical axis has a relatively small impact on the final image, the actual measurement has a certain degree of redundancy. A control matrix for the redundant degrees of freedom is constructed using the least squares principle, and digital adaptive correction of the mirror surface is achieved through optimization in the least squares sense. Specifically, the system wavefront can be represented using the orthogonal basis of Zernike polynomials. Through calibration and principal component analysis, a mapping relationship between the six-dimensional spatial position and the final Zernike polynomial is established, that is, the Zernike polynomial of the final system incident wavefront is directly obtained through the acceleration signal.

[0032] Sixth: Optional ultra-long-time integration for extremely faint celestial objects. This invention can employ a corresponding integration time, that is, continuously calculating the real-time surface features of the system during this process, linearly accumulating these surface features, and finally generating a point spread function that matches the long-time integration, and ultimately achieving deconvolution of the image.

[0033] 7. Furthermore, the laser ranging component in the optical truss can also be implemented in a transmission manner. By varying the optical path length of the lenses along the optical path, the pose of the transmission element can be controlled. Based on this, the system's transfer function and point spread function are constructed, ultimately achieving digital deconvolution. Internal system measurements via the optical truss avoid degradation in system alignment and imaging quality caused by external interference, while also enabling condition measurement during the observation process, thus improving observation efficiency.

[0034] The imaging process of large-aperture optical elements can be approximated as the convolution of the object's light field information and the point spread function. Common optical systems use the Airy disk as the convolution kernel, while the kernel of a large-aperture stitched system is determined by the state of the optical system. This paper uses an optical truss to solve for the segmented primary mirror shape and optical element alignment, thereby estimating the wavefront. (The imaging of a large-aperture, wide-field-of-view telescope is achieved through convolutional processing. This utilizes an all-optical image convolution system (with the primary mirror being a spatial light modulator, combined with pixel merging), employing a simple convolutional neural network to perform optical calculations on gravitational lensing. The output is the solution itself, requiring no further processing. Due to the low pixel resolution of the large aperture and wide-field-of-view telescope, active optics can be used for wavefront modulation to highlight edges and suppress noise. For experimental verification, deformable mirrors combined with extended targets are used to achieve aberration correction.)

[0035] refer to Figure 2 and Figure 3 The optical truss of the telescope system in this application can achieve component attitude calculation using only distance variables. By inputting the current measurement results of the optical truss into the theoretical model, the current system misalignment can be obtained; the drive mechanism is then controlled based on the obtained current misalignment.

[0036] "Optical truss" refers to a method of controlling the position of components using distance measurement. Because it resembles a mechanical truss composed of rods, it is called an "Optics Truss." Based on the concept of optical trusses, real-time coarse alignment of large-aperture, wide-field-of-view telescopes can be achieved, ensuring the smooth operation of active optics. Distance measurement is accomplished through modulated laser carrier signals. Reflectors can use prisms, cat's-eye lenses, and diffuse reflective surfaces (but these require light-colored surfaces, and the distance is also limited). This not only makes them small and easy to arrange but also provides better environmental adaptability.

[0037] Optical trusses can solve for component attitude using only distance variables. The current measurement results from the optical truss are input into the theoretical model to obtain the current system misalignment; the drive mechanism is then controlled based on this misalignment. Through redundant measurements and cross-comparisons of acceleration and ranging, the rigid body assumption offset can be obtained, enabling the sensing of deformation under thermal loads. In other words, by monitoring the drift of optical ranging over long timescales, real-time monitoring of the distance and relative position between components can be achieved, correcting the decrease in system detection capability caused by thermal drift.

[0038] Model Derivation: The acceleration signals are solved jointly. Based on the principles of rigid body kinematics, the linear acceleration at any point in the moving coordinate system can be expressed as:

[0039] in, To increase the acceleration, Let p be the position vector of point p in the moving coordinate system. These are angular acceleration and angular velocity, respectively. A single-axis accelerometer is located at point P. Assuming the optical axis direction is the sensitive axis direction, the output value of the optical axis direction obtained at each measuring point is:

[0040] To reduce computational complexity, redundant measurements are performed using multi-axis accelerometers, and linear combinations can be used to make...

[0041]

[0042] The model can be linearized using the cross product equivalent expression (1) in matrix theory, as shown in formula (2): (1) (2) Meanwhile, since the degree of freedom of rotation about the optical axis can be ignored, For known quantities ,therefore.

[0043]

[0044] First, consider the jitter along the normal direction of the mirror. Assume that the directions of the sensitive axes of several accelerometers are all parallel to the mirror normal, and that the geometric centers of the three measuring points coincide with the center of mass of the mirror. Therefore: Adding the signals from the three accelerometers together gives:

[0045] As the previous derivation shows, accelerometers can relatively easily have their geometric center positioned at a point on the system, which is quite difficult for gyroscopes. Angular velocity can be obtained, and angular displacement can be obtained through a single integration.

[0046] Fusion analysis of accelerometers: By using two distance measurement methods to determine a fixed distance, and then using an accelerometer to measure angle information, the two sets of information can be fused. This is achieved by setting the accelerometer... and The point closest to the distant point is determined by comparing the accelerometer signal with the laser ranging signal, based on the differences in time scale characteristics. This includes expansion caused by separable force and thermal loads (lower time frequency) and changes in optical path due to airflow disturbances (higher time frequency).

[0047] Regarding evaluation metrics, how to characterize and evaluate system stability is the premise and foundation of this research. The system modulation transfer function (MTF) has a direct mapping relationship with traditional optical system quality evaluation methods. This project aims to establish a unified characterization standard for high-frequency stability in the system based on the MTF. This will allow for the acquisition of a regular expression of optical system quality degradation. The diffusion function at time t: (3) in The dynamic point spread function characterizes stability. The time for integration.

[0048] Based on the relationship between PSF and MTF: (Fourier Transform) (4) Modulation transfer function characterizing dynamic stability

[0049] in For spatial frequency, For integration time. (The first...) The setting of each link Overall Equation (5) can be used to characterize high-frequency stability. (5) Where N represents the total number of system components. Based on the static evaluation of the optical system, the relationship between mechanical resonance, system control, and optics can be established using the dynamic transfer function. Ultimately, this achieves an effective characterization of multi-temporal boundary interaction effects in the spatiotemporal frequency domain.

[0050] The optical truss samples the system pose under jitter during exposure and sets the position based on the point spread function. Let represent the adjoint transformation matrix. (6) The original coordinate system represents the direction in the new coordinate system, and c and s represent the "cos" and "sin" functions, respectively. (7) The transformed sub-mirror shape is After translating it, the point spread function (PSF) that generates motion blur for point K in the image plane is: (8) The effect of jitter can be removed by using deconvolution. The acceleration signal of the whole system can be obtained from the accelerometer located at the bottom of the secondary mirror chamber, and the displacement signal can be obtained using equation (7), such as Figure 3 As shown, the power spectrum of the signal is as follows: Figure 6 As shown: For the correction control algorithm, since the active optical control bandwidth is lower than the system resonance, the interaction between the structure and the controller does not need to be considered.

[0051] (9) in The sensor output is u, and the control input is 'u'. This is called the influence matrix. For large-aperture spliced ​​mirrors, the discrete-time integral controller becomes: (10) Where Φ* represents the pseudo-inverse matrix of the poke matrix, also known as the reconstruction matrix, and μ is the adaptive gain. Generally, when the number of sensor measurements exceeds the number of inputs, the pseudo-inverse process provides the least-squares solution for the control input required to correct aberrations. Here, the accelerometer has redundancy, but the control model of the system is simplified through directional combination. Therefore, the system is achievable. A sinusoidal perturbation signal (determined amplitude, random phase) is applied to each sub-mirror to simulate the actual perturbation, simulating perturbations of different amplitudes. Real-time wavefronts are acquired through the optical truss and deconvolution calculations are performed. The wavefront and correction effects are utilized... The following are specific application examples: The process of deconvolution through wavefront settlement, such as Figure 5 As shown, a simulated interferogram is first formed through convolution, and then deconvolution is performed based on the wavefront measurement results obtained through long-term integration. Specifically, the generated convolutional image reflects the influence of instantaneous wavefront perturbations, while deconvolution requires several long-term integrations to average the impact of detection errors, ensuring the robustness and stability of the correction process.

[0052] like Figures 6 to 10 The figure shows a comparison between real-time wavefront sensing and the wavefront propagation results after 200 frames of averaging, and the relationship with the point spread function.

[0053] See Figure 13-14 Regarding the passive damping structure, it includes an air cushion and a steel wire damper, forming a coupled passive main unit system. In semi-active damping, this magnetofluid is injected into a hydraulic cylinder, which is circulated and can generate damping. Then, the outer ring of the entire system has coils. The coils change the viscosity and hardness of the magnetofluid through different electric fields, and regulate the damping by controlling external disturbances.

[0054] In terms of intelligent suppression, the splicing process uses a voice coil architecture. It utilizes the feedback from the encoder value to suppress high-frequency information. The encoder feedback undergoes temporal filtering at lower frequencies to close the loop for position determination. Then, higher spatial temporal and frequency information, along with the electronically controlled voice coil, is used to suppress vibration, thus achieving jitter suppression. On the left is an airbag, and next to it is a rigid assembly resembling a steel wool pad. There's also a piston with a slot or hole in the center for adjustment.

[0055] It contains a magnetofluid, and the surrounding magnetic field is controlled by changing the current in the outer coil, achieving semi-active regulation. Its function is that if it is not actively regulated by the outside, it will easily become unstable.

[0056] See Figure 13-14 The parallel terminal is also a slot, containing magnetohydrodynamic fluid and a coil. By adjusting the current, the passive damping is adjusted.

[0057] Example 2 According to another embodiment of the present invention, an adjustment device for improving the imaging resolution of a large-aperture telescope system is provided, see [link to previous document]. Figure 11 ,include: Mounting module 100 is used to place at least three accelerometers after each sub-mirror of the segmented splicing telescope system. The measurement module 200 is used to perform precision measurement of the initial position of each sub-mirror using a spatial coordinate measurement device, and to perform high-frequency measurement of the three-dimensional position of all sub-mirrors based on the position of each sub-mirror and the calibrated sensitive axis direction. The system construction module 300 is used to construct a real-time overall mirror surface shape expression through the accelerometer on each splicing sub-mirror, and based on the constructed overall mirror surface shape expression combined with the working wavelength, construct a new surface shape measurement system that does not require direct imaging and exposure integration. The image processing module 400 is used to obtain the dynamic surface profile of the telescope system through the accelerometer based on the new surface profile measurement system. It combines the dynamic surface profile with the propagation law of Fourier optics to perform optical inversion, construct the instantaneous point spread function of the telescope system, and perform image deconvolution using the point spread function to obtain higher resolution imaging effect.

[0058] The present invention relates to a method and apparatus for improving the imaging resolution of a large-aperture telescope system. This application obtains the dynamic surface profile of the telescope system from an accelerometer, combines the dynamic surface profile with the propagation laws of Fourier optics to perform optical inversion, constructs the instantaneous point spread function of the system, and uses this point spread function to perform image deconvolution to obtain a higher resolution imaging effect.

[0059] Example 3 Based on the above-described method for adjusting the imaging resolution of a large-aperture telescope system, this embodiment provides a computer-readable storage medium storing one or more programs that can be executed by one or more processors to implement the steps in the method for adjusting the imaging resolution of a large-aperture telescope system as described in the above embodiment.

[0060] Example 4 A terminal device includes: a processor, a memory, and a communication bus; the memory stores a computer-readable program that can be executed by the processor; the communication bus enables communication between the processor and the memory; when the processor executes the computer-readable program, it implements the steps in the above-described method for adjusting the imaging resolution of a large-aperture telescope system.

[0061] Based on the aforementioned method for improving imaging resolution in large-aperture telescope systems, this application provides a terminal device, such as... Figure 11 As shown, it includes at least one processor 20; a display screen 21; and a memory 22, and may also include a communications interface 23 and a bus 24. The processor 20, display screen 21, memory 22, and communications interface 23 can communicate with each other via the bus 24. The display screen 21 is configured to display a preset user guide interface in the initial setup mode. The communications interface 23 can transmit information. The processor 20 can invoke logical instructions in the memory 22 to execute the methods described in the above embodiments.

[0062] Furthermore, the logical instructions in the aforementioned memory 22 can be implemented as software functional units and, when sold or used as independent products, can be stored in a computer-readable storage medium.

[0063] The memory 22, as a computer-readable storage medium, can be configured to store software programs, computer-executable programs, such as program instructions or modules corresponding to the methods in the embodiments of this disclosure. The processor 20 executes functional applications and data processing by running the software programs, instructions, or modules stored in the memory 22, thereby implementing the methods in the above embodiments.

[0064] The memory 22 may include a program storage area and a data storage area. The program storage area may store the operating system and applications required for at least one function; the data storage area may store data created based on the use of the terminal device. Furthermore, the memory 22 may include high-speed random access memory (RAM) and may also include non-volatile memory, such as a USB flash drive, a portable hard drive, or a read-only memory (ROM). It can be a medium that can store program code, such as ROM, RAM, magnetic disks or optical disks, or it can be a temporary storage medium.

[0065] Furthermore, the specific process of loading and executing multiple instruction processors in the aforementioned storage medium and terminal device has been described in detail in the above method, and will not be repeated here.

[0066] The above description is only a preferred embodiment of the present invention. It should be noted that for those skilled in the art, several improvements and modifications can be made without departing from the principle of the present invention, and these improvements and modifications should also be considered within the scope of protection of the present invention.

Claims

1. A method for adjusting the imaging resolution of a large-aperture telescope system, characterized in that, Includes the following steps: At least three accelerometers are placed after each sub-mirror in the segmented splicing telescope system; The initial position of each sub-mirror is accurately measured using a spatial coordinate measuring device, and the spatial three-dimensional position of all sub-mirrors is measured at high frequency based on the position of each sub-mirror and the calibrated sensitive axis direction. By using the accelerometer on each of the spliced ​​sub-mirrors, a real-time overall mirror surface shape expression is constructed. Based on the constructed overall mirror surface shape expression and the working wavelength, a new surface shape measurement system that does not require direct imaging and exposure integration is constructed. Based on the new surface shape measurement system, the dynamic surface shape of the telescope system obtained by the accelerometer is combined with the propagation law of Fourier optics to perform optical inversion, construct the instantaneous point spread function of the telescope system, and perform image deconvolution with the point spread function to obtain a higher resolution imaging effect.

2. The method for improving imaging resolution of a telescope system according to claim 1, characterized in that, The specific steps of accurately measuring the initial position of each sub-mirror using a spatial coordinate measuring device are as follows: The initial position of each sub-mirror is precisely measured using a coordinate measuring machine.

3. The method for adjusting the imaging resolution of the telescope system according to claim 1, characterized in that, The method further includes: The spatial positions of the primary mirror, secondary mirror, and final mirror of the telescope system are measured using laser ranging.

4. The method for adjusting the imaging resolution of the telescope system according to claim 1, characterized in that, After accurately measuring the initial position of each sub-mirror using a spatial coordinate measuring device, and performing high-frequency measurements of the three-dimensional spatial positions of all sub-mirrors based on the position of each sub-mirror and the calibrated sensitive axis direction, the method further includes: The pose of each of the sub-mirrors is measured, and the real-time feedback of the pose measurement results reduces the jitter of the telescope system and its impact on the final image contrast.

5. The method for improving imaging resolution of a telescope system according to claim 1, characterized in that, Each of the aforementioned sub-mirrors retains six degrees of freedom.

6. The method for adjusting the imaging resolution of a telescope system according to claim 1, characterized in that, The expression for the point spread function is: in The dynamic point spread function characterizes stability. Let t be the integration time, and t be the diffusion function at that time point.

7. The method for adjusting the imaging resolution of the telescope system according to claim 6, characterized in that, Performing a Fourier transform on the point spread function yields the transformed expression: Modulation transfer function characterizing dynamic stability ,in For spatial frequency, For the integration time, the first The setting of each link The overall formula is as follows, which can be used to characterize high-frequency stability: Where N is the total number of system components, the relationship between mechanical resonance, system control and optics can be established by using the dynamic transfer function based on the static evaluation of the optical system; ultimately, the effective characterization of multi-temporal boundary interaction effects in the spatiotemporal frequency domain can be achieved.

8. A method for adjusting the imaging resolution of a telescope system, characterized in that, include: The mounting module is used to place at least three accelerometers after each sub-mirror in a segmented splicing telescope system. The measurement module is used to accurately measure the initial position of each sub-mirror using a spatial coordinate measuring device, and to perform high-frequency measurements of the three-dimensional spatial position of all the sub-mirrors based on the position of each sub-mirror and the calibrated sensitive axis direction. The system construction module is used to construct a real-time overall mirror surface shape expression by using the accelerometer on each of the spliced ​​sub-mirrors, and to construct a new surface shape measurement system that does not require direct imaging and exposure integration based on the constructed overall mirror surface shape expression and the working wavelength. The image processing module is used to perform optical inversion based on the dynamic surface profile of the telescope system obtained by the accelerometer, combined with the propagation law of Fourier optics, to construct the instantaneous point spread function of the telescope system, and to perform image deconvolution using the point spread function to obtain a higher resolution imaging effect.

9. A computer-readable medium, characterized in that, The computer-readable storage medium stores one or more programs, which can be executed by one or more processors to implement the steps in the adjustment method for improving imaging resolution of the telescope system as described in any one of claims 1-7.

10. A terminal device, characterized in that, include: Processor, memory, and communication bus; The memory stores a computer-readable program that can be executed by the processor; The communication bus enables communication between the processor and the memory; When the processor executes the computer-readable program, it implements the steps in the adjustment method for improving imaging resolution of the telescope system as described in any one of claims 1-7.

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