Telescope system simulation method and device for ultra-high contrast imager testing

Abstract

The present invention discloses a telescope system simulation method and device for testing ultra-high contrast imagers. The method comprises: collimating a white light point source, reflecting it onto a first deformable mirror, and then reflecting it again before being incident on a second deformable mirror; controlling the actuator unit matrices of the first and second deformable mirrors to move row by row or column by column on a phase screen image simulating upper atmospheric turbulence and near-surface atmospheric turbulence, respectively, and establishing a conversion relationship between the pixel values ​​of the phase screen image and the travel of the deformable mirror actuators; and causing parallel light containing wavefront distortion to be reflected by the second deformable mirror and pass through a telescope pupil simulation aperture, where it is converged to form a primary focus, and the scaled parallel light is converged to form a secondary focus. The present invention can simulate the dynamic disturbances caused by upper atmospheric turbulence and near-surface atmospheric turbulence on the incident light wavefront during ground-based astronomical telescope imaging observations, and can also simulate the pupil shape and position of an astronomical telescope.

Description

Technical Field

[0001] The present invention belongs to the field of exoplanet imaging detection technology and ultra-high contrast imaging instruments, and in particular relates to a telescope system simulation method and device for ultra-high contrast imager testing. Background Art

[0002] As a scientific terminal on an astronomical telescope, an ultra-high-contrast imaging instrument is not only a powerful tool for detecting and discovering exoplanets, but also holds important significance for characterizing planetary physical parameters and searching for and confirming signatures of extraterrestrial life. Once an ultra-high-contrast imaging instrument is developed and officially docked with a telescope for observation, its performance must first be thoroughly tested and calibrated in the laboratory to accurately predict its performance and state in actual observations. Therefore, it is imperative to develop a telescope system simulation method and device suitable for testing ultra-high-contrast imaging instruments. Analysis has shown that these methods and devices should meet the following requirements: 1) simulate the dynamic perturbations of upper and lower atmospheric turbulence encountered during ground-based observations; 2) simulate the shape and position of the astronomical telescope's pupil; 3) form a benchmark for docking with the ultra-high-contrast imaging instrument; and 4) optically transfer the telescope's simulated pupil so that it can ultimately be conjugated to the wavefront correction unit within the ultra-high-contrast imaging instrument.

[0003] Chinese patent publication number CN105610493A discloses a system and method for simulating atmospheric turbulence based on inverse adaptive technology. This system addresses the challenges of satellite-to-ground laser communications, requiring turbulence simulation systems to adapt to multiple wavelengths, maintain polarization, and maintain a small footprint. The system comprises a wavefront perturbation module, a wavefront detection module, and a control module. Based on the wavefront detection module's measurement results, it establishes a lookup table that correlates voltage with turbulence arrival angle fluctuations and coherence length. A micro-deformable mirror is used to simulate the localized distortion of the wavefront caused by turbulence.

[0004] Chinese patent publication number CN107040308A discloses a laser atmospheric transmission turbulence simulation and far-field spot detection instrument. This instrument addresses the challenges of simulating atmospheric turbulence and vibration during laser far-field transmission, and detecting laser far-field spot in both turbulent and non-turbulent conditions, both in the presence and absence of turbulence. The instrument utilizes a turbulence and vibration simulation component, a far-field spot detection component, and optical components. Software injects measured atmospheric parameters and uses a deformable mirror to simulate the effects of atmospheric turbulence.

[0005] Chinese patent publication number CN107796594A discloses an atmospheric turbulence simulator based on a spatial light modulator (SLM). This approach addresses the challenges in atmospheric optics and optical communications, where simulation devices are difficult to flexibly adjust to varying atmospheric conditions and beam propagation distances, leading to limited practicality. The device described in this invention simulates atmospheric turbulence using three coaxial, collinear SLMs.

[0006] The invention used as an example above does not have the ability to simulate atmospheric turbulence at different altitudes, does not contain information on the shape and position of the pupil of the astronomical telescope, has no benchmark for docking with ultra-high contrast imaging instruments, and does not involve optical transmission of the simulated pupil of the telescope. Therefore, it cannot meet the actual testing needs of ultra-high contrast imaging instruments. Summary of the Invention

[0007] In order to solve the problem of testing ultra-high contrast imaging instruments, the present invention proposes a telescope system simulation method and device for ultra-high contrast imager testing.

[0008] To achieve the above object, the present invention provides a telescope system simulation method for ultra-high contrast imager testing, comprising the following steps:

[0009] Step 1: Generate a point source of white light to simulate incident starlight;

[0010] Step 2: collimate the white light point source into parallel light, and then reflect the parallel light onto the first deformable mirror;

[0011] Step 3: The light is reflected by the first deformable mirror and then incident on the second deformable mirror;

[0012] Step 4: Use a computer to read the phase screen images of simulated upper atmospheric turbulence and near-ground atmospheric turbulence respectively;

[0013] Step 5: Controlling the actuator unit matrices of the first deformable mirror and the second deformable mirror to move row by row or column by column on a phase screen image simulating upper atmospheric turbulence and near-ground atmospheric turbulence, respectively, and establishing a conversion relationship between the pixel values ​​of the phase screen image and the travel amount of the deformable mirror actuator;

[0014] Step 6: The parallel light with wavefront distortion is reflected by the second deformable mirror and then passes through the telescope pupil simulation aperture, wherein the telescope pupil simulation aperture is used to simulate the pupil shape and pupil position of an astronomical telescope;

[0015] Step 7: The parallel light containing wavefront distortion and the shape of the telescope's simulated pupil is converged to form a primary focus, and then collimated into parallel light to achieve scaling of the telescope's simulated pupil size;

[0016] Step 8: The scaled parallel light is converged to form a secondary focus. The ultra-high contrast imaging instrument uses the secondary focus as a docking reference. After the optical transfer according to steps 6 to 8, the telescope simulated pupil is conjugated to the wavefront correction unit by the collimating lens inside the ultra-high contrast imaging instrument.

[0017] Furthermore, in step 3, the first deformable mirror and the second deformable mirror are used to simulate the disturbance effects of high-level atmospheric turbulence and near-ground atmospheric turbulence, respectively.

[0018] Furthermore, in step 4, the actuator unit matrices of the first deformable mirror and the second deformable mirror are respectively mapped to the phase screen image matrix simulating high-altitude atmospheric turbulence and near-ground atmospheric turbulence. There is no requirement for the initial alignment position between the two matrix elements and it can be any position.

[0019] Furthermore, in step 5, the stroke amounts of the first deformable mirror and the second deformable mirror actuator are obtained by converting the numerical values ​​of the phase screen image pixels simulating high-altitude atmospheric turbulence and near-ground atmospheric turbulence respectively, and then the real-time driving voltage signals of the actuators of the first deformable mirror and the second deformable mirror are obtained respectively based on the relationship between the input control signal range of the first deformable mirror and the second deformable mirror and their maximum stroke amounts.

[0020] Furthermore, in step 6, when simulating the pupil of an astronomical telescope with a single primary mirror, the telescope pupil simulation aperture is realized by opening up a partial area on an opaque flat plate, including an outer circle, an inner circle and a crosshair, the outer circle and the inner circle are concentric, the center of the crosshairs coincides with the center of the circle and symmetrically passes through the outer circle and the inner circle; wherein, the area between the outer circle and the inner circle is translucent, simulating the light-transmitting area of ​​the telescope primary mirror; the inner circle is opaque, simulating the obstruction of the telescope secondary mirror projected on the primary mirror; the crosshairs are opaque, simulating the obstruction of the telescope secondary mirror support ribs projected on the primary mirror.

[0021] The present invention also provides a telescope system simulation device for testing an ultra-high contrast imager, comprising a laser-driven white light source, an optical fiber, a microscope objective, a pinhole, a first glued collimating lens, a first plane reflector, a first deformable mirror, a second plane reflector, a second deformable mirror, a telescope pupil simulation aperture, a first glued imaging lens, a third plane reflector, a second glued collimating lens, and a second glued imaging lens, which are arranged in sequence along the optical path. The device also comprises a first deformable mirror controller and a second deformable mirror controller connected to a computer, and the first deformable mirror controller and the second deformable mirror controller respectively drive the displacement of the actuators of the first deformable mirror and the second deformable mirror.

[0022] Furthermore, after the laser-driven white light source is output through optical fiber coupling, it is converged by the microscope objective lens onto the pinhole to generate a white light point source, simulating incident starlight. The first glued collimating lens collimates the white light point source into parallel light, which is then reflected by the first plane mirror to the first deformable mirror. The first deformable mirror reflects the light to the second plane mirror, and then reflects it to the second deformable mirror. The first deformable mirror and the second deformable mirror are used to simulate the disturbance effects of high-altitude atmospheric turbulence and near-ground atmospheric turbulence, respectively. The parallel light containing wavefront distortion passes through the telescope pupil simulation aperture, which is used to simulate the pupil shape and pupil position of an astronomical telescope. The parallel light containing wavefront distortion and the telescope simulated pupil shape is converged by the first glued imaging lens to form a primary focus, and then reflected by the third plane mirror and collimated into parallel light by the second glued collimating lens, thereby scaling the size of the telescope simulated pupil. The scaled parallel light is converged by the second glued imaging lens to form a secondary focus, and the ultra-high contrast imaging instrument uses the secondary focus as a docking reference.

[0023] Furthermore, the telescope pupil simulation aperture is located at a position of one focal length of the first cemented imaging lens, the distance between the second cemented collimating lens and the second cemented imaging lens is equal to the sum of their focal lengths, and the F number of the secondary focus (F number = f R2 / d pupil_mag , where f R2 is the focal length of the second cemented imaging lens, d pupil_mag The simulated pupil size of the telescope after scaling is less than or equal to the F number of the collimating lens inside the ultra-high contrast imaging instrument. The secondary focus is located at a position one focal length in front of the collimating lens inside the ultra-high contrast imaging instrument. The wavefront correction unit inside the ultra-high contrast imaging instrument is located at a position one focal length behind the collimating lens. The simulated pupil of the telescope is ultimately conjugated to the wavefront correction unit.

[0024] The beneficial effects of the present invention are:

[0025] 1. The simulation method and device proposed in this invention can simulate the dynamic disturbances caused by upper atmospheric turbulence and near-surface atmospheric turbulence on the incident light wavefront during imaging observations by ground-based astronomical telescopes, and can test the working performance of ultra-high contrast imaging instruments more closely to actual observation conditions.

[0026] 2. The simulation method and device proposed in the present invention can simulate the pupil shape and pupil position of an astronomical telescope, and can accurately estimate the imaging contrast of ultra-high contrast imaging instruments when using different telescopes.

[0027] 3. The simulation method and device proposed in the present invention are specifically optimized for the docking reference and pupil optical transfer requirements of ultra-high contrast imaging instruments, facilitating the docking test of ultra-high contrast imaging instruments. BRIEF DESCRIPTION OF THE DRAWINGS

[0028] Figure 1 This is the process flow of the telescope system simulation method proposed in the present invention for ultra-high contrast imager testing.

[0029] Figure 2 This is a schematic diagram of the structure of a telescope system simulation device for ultra-high contrast imager testing proposed in the embodiment;

[0030] Figure numerals: 1: laser-driven white light source; 2: optical fiber; 3: microscope objective lens; 4: pinhole; 5: first glued collimating lens; 6: first plane mirror; 7: first deformable mirror; 8: second plane mirror; 9: second deformable mirror; 10: telescope pupil simulation aperture; 11: first glued imaging lens; 12: third plane mirror; 13: second glued collimating lens; 14: second glued imaging lens; 15: first deformable mirror controller; 16: second deformable mirror controller. DETAILED DESCRIPTION

[0031] In order to make the objectives, technical solutions and advantages of the present invention more clearly understood, the present invention is further described in detail below with reference to the accompanying drawings and embodiments. It should be understood that the specific embodiments described herein are only intended to illustrate the present invention and are not intended to limit the present invention. In addition, the technical features involved in the various embodiments of the present invention described below may be combined with each other as long as they do not conflict with each other.

[0032] The telescope system simulation method for ultra-high contrast imager testing of the present invention is as follows Figure 1 As shown, the following steps are included:

[0033] Step 1: After the laser-driven white light source is coupled to the optical fiber, it is focused on the pinhole by the microscope objective lens to produce a white light point source, simulating the incident starlight;

[0034] Step 2: The first cemented collimating lens collimates the white light point source into parallel light, and then the first plane reflector reflects the parallel light to the first deformable mirror;

[0035] Step 3: After being reflected by the first deformable mirror, the light is incident on the second deformable mirror through the second plane reflector.

[0036] Furthermore, the first deformable mirror and the second deformable mirror are used to simulate the disturbance effects of high-altitude atmospheric turbulence and near-ground atmospheric turbulence respectively.

[0037] Furthermore, the actuator units of the first deformable mirror and the second deformable mirror are arranged in K×K and L×L arrays respectively, and the matrices thereof are expressed as follows:

[0038]

[0039] Where DM1 and DM2 are the actuator unit arrangement matrices of the first deformable mirror and the second deformable mirror, respectively. E represents the presence of an actuator at that position, and 0 represents the absence of an actuator at that position. i, j, m, and n are the column and row numbers of the first deformable mirror actuator, respectively. i', j', m', and n' are the column and row numbers of the second deformable mirror actuator, respectively.

[0040] Step 4: Use a computer to read the phase screen images of simulated upper atmospheric turbulence and near-ground atmospheric turbulence respectively.

[0041] Furthermore, the phase screen image size for simulating upper atmospheric turbulence is M×N (M>>K, N≥K or N>>K, M≥K), and the phase screen image size for simulating near-surface atmospheric turbulence is P×Q (P>>L, Q≥L or Q>>L, P≥L), and their image matrices are expressed as:

[0042]

[0043] Where, PS H and PS G are the phase screen image matrices simulating high-altitude atmospheric turbulence and near-ground atmospheric turbulence, respectively. A and B represent the values ​​of the phase screen image pixels, and the unit is phase.

[0044] Furthermore, the actuator unit matrices of the first deformable mirror and the second deformable mirror are mapped onto phase screen image matrices simulating upper atmospheric turbulence and near-ground atmospheric turbulence, respectively. The initial alignment position between the two matrix elements is not required and can be any position.

[0045] Step 5: Control the actuator unit matrices of the first deformable mirror and the second deformable mirror to move row by row or column by column on the phase screen image simulating high-altitude atmospheric turbulence and near-ground atmospheric turbulence, respectively.

[0046] Furthermore, a conversion relationship between the phase screen image pixel value and the deformable mirror actuator stroke is established:

[0047]

[0048] Where Str1(i,j) and PS H (i, j) are the stroke of the actuator at the i-th row and j-th column of the first deformable mirror, and the value of the pixel at the i-th row and j-th column of the phase screen image simulating high-altitude atmospheric turbulence, Str2(i′, j′) and PS G(i′, j′) are the stroke of the actuator at the i′th row and j′th column of the second deformable mirror and the value of the pixel at the i′th row and j′th column of the phase screen image simulating near-ground atmospheric turbulence, respectively. λ is the wavelength.

[0049] Furthermore, the driving voltage ranges of the first deformable mirror and the second deformable mirror are [-V1, +V1] and [-V2, +V2], respectively, and the corresponding actuator stroke ranges are [-S1 / 2, +S1 / 2] and [-S2 / 2, +S2 / 2], respectively, where S1 and S2 are the maximum strokes of the first deformable mirror and the second deformable mirror actuators, respectively. The real-time driving voltage signals of the actuators of the first deformable mirror and the second deformable mirror can be obtained as follows:

[0050]

[0051] Where Sig1(i, j) and Sig2(i′, j′) are the driving voltage values ​​of the actuator at the i-th row and j-th column of the first deformable mirror and the driving voltage values ​​of the actuator at the i′th row and j′th column of the second deformable mirror, respectively.

[0052] Step 6: The parallel light with wavefront distortion is reflected by the second deformable mirror and then passes through the telescope pupil simulation aperture, which is used to simulate the pupil shape and pupil position of an astronomical telescope.

[0053] Furthermore, when simulating the pupil of an astronomical telescope with a single primary mirror, the telescope pupil simulation aperture is realized by opening up part of the area on an opaque flat plate, including an outer circle, an inner circle and a crosshair, the outer circle and the inner circle are concentric, the center of the crosshair coincides with the center of the circle and symmetrically passes through the outer circle and the inner circle; wherein, the area between the outer circle and the inner circle is translucent, simulating the light-transmitting area of ​​the telescope primary mirror; the inner circle is opaque, simulating the obstruction of the telescope secondary mirror projected on the primary mirror; the crosshairs are opaque, simulating the obstruction of the telescope secondary mirror support ribs projected on the primary mirror.

[0054] Furthermore, the outer diameter d Outer Less than or equal to the incident parallel light diameter, the inner circle diameter d Inner =d Outer CO, where CO is the central obscuration ratio of the telescope, CO = D M2 / D M1 , where D M1 and D M2 are the diameters of the primary mirror M1 and the secondary mirror M2 of the telescope, and the crosshair width d Spider =D Spider ·(d Outer / D M1 ), where D Spideris the width of the telescope's secondary mirror support rib projected onto the primary mirror, and the telescope pupil simulation aperture is located at a position of one focal length of the first cemented imaging lens;

[0055] Step 7: The parallel light containing wavefront distortion and the shape of the telescope's simulated pupil is converged by the first cemented imaging lens to form a primary focus, and then reflected by the third plane mirror and collimated by the second cemented collimating lens into parallel light, thereby achieving the scaling of the telescope's simulated pupil size.

[0056] Furthermore, the simulated pupil size d of the scaled telescope is pupil_mag =d Outer ·(f C2 / f R1 ), where f C2 and f R1 are the focal lengths of the first cemented imaging lens and the second cemented collimating lens, respectively;

[0057] Step 8: The scaled parallel light is converged by the second glued imaging lens to form a secondary focus, and the ultra-high contrast imaging instrument uses the secondary focus as a docking reference.

[0058] Furthermore, the distance between the second cemented collimating lens and the second cemented imaging lens is equal to the sum of their focal lengths, and the F number of the secondary focus (F number = f R2 / d pupil_mag , where f R2 is the focal length of the second cemented imaging lens, d pupil_mag is the scaled telescope simulated pupil size) is less than or equal to the F number of the collimating lens inside the ultra-high contrast imaging instrument, the secondary focus is located at a position one focal length in front of the collimating lens inside the ultra-high contrast imaging instrument, and the wavefront correction unit inside the ultra-high contrast imaging instrument is located at a position one focal length behind the collimating lens thereof. After the optical transfer according to steps 6 to 8, the simulated pupil of the telescope is finally conjugated to the wavefront correction unit.

[0059] In this embodiment, the specific structure of the telescope system simulation device for ultra-high contrast imager testing is as follows: Figure 2As shown, the simulation device includes a laser-driven white light source 1, an optical fiber 2, a microscope objective lens 3, a pinhole 4, a first cemented collimating lens 5, a first plane reflector 6, a first deformable mirror 7, a second plane reflector 8, a second deformable mirror 9, a telescope pupil simulation aperture 10, a first cemented imaging lens 11, a third plane reflector 12, a second cemented collimating lens 13, a second cemented imaging lens 14, a first deformable mirror controller 15, and a second deformable mirror controller 16. The first deformable mirror 7 and the second deformable mirror 9 are used to simulate the disturbance effects of upper atmospheric turbulence and near-surface atmospheric turbulence, respectively. The telescope pupil simulation aperture 10 is used to simulate the pupil shape and position of an astronomical telescope. The first cemented imaging lens 11 forms a primary focus. The second cemented collimating lens 13 scales the size of the simulated telescope pupil. The second cemented imaging lens 14 forms a secondary focus. The first deformable mirror controller 15 and the second deformable mirror controller 16 drive the displacement of the actuators of the first deformable mirror 7 and the second deformable mirror 9, respectively.

[0060] The laser-driven white light source 1 is coupled to the optical fiber 2 and outputs a spectrum covering 350 to 2500 nm. The microscope objective 3 focuses the output light of the optical fiber 2 to the pinhole 4 to generate a white light point source. The pinhole diameter is 2 to 5 μm.

[0061] The first cemented collimating lens 5 has an aperture of 25.4 to 50.8 mm and a focal length range of 200 to 500 mm. It collimates the white light point source into parallel light. This light is then reflected by the first plane reflector 6 onto the first deformable mirror 7, which has an aperture of 25.4 to 50.8 mm and folds the optical path. Based on existing laboratory equipment, the first deformable mirror 7 has a clear aperture of 13.5 mm and 97 actuators arranged in an 11x11 array. The actuators have a maximum stroke of 60 μm, designed to simulate the disturbances of upper atmospheric turbulence.

[0062] First deformable mirror 7 reflects light onto first plane mirror 8, which then reflects it onto second deformable mirror 9. Based on existing laboratory equipment, second deformable mirror 9 has a 13.5mm aperture and 97 actuators arranged in an 11x11 array. The actuators have a maximum stroke of 60μm, simulating near-surface atmospheric turbulence. The phase screen image size for simulating upper atmospheric turbulence is 11x11000 or 11000x11, and for simulating near-surface atmospheric turbulence, the image size is 11x11000 or 11000x11, with a wavelength of 632.8nm to 2.2μm.

[0063] The telescope pupil simulation diaphragm 10 takes several typical 2-4 meter aperture astronomical telescopes at home and abroad as examples, including: 1) the pupil simulation diaphragm of the 2.4-meter telescope at the Yunnan Astronomical Observatory, whose outer and inner diameters are 13.50 mm and 3.92 mm, respectively, and the crosshairs width is 0.1-0.2 mm; 2) the pupil simulation diaphragm of the 3.6-meter NTT telescope at the La Silla Observatory in Chile, whose outer and inner diameters are 13.50 mm and 3.10 mm, respectively, and the crosshairs width is 0.1-0.2 mm; 3) the pupil simulation diaphragm of the 3.5-meter ARC telescope at the Apache Point Observatory in the United States, whose outer and inner diameters are 13.50 mm and 2.88 mm, respectively, and the crosshairs width is 0.1-0.2 mm; and 4) the pupil simulation diaphragm of the 3.58-meter TNG telescope at the Roque de los Muchachos Observatory in Spain, whose outer and inner diameters are 13.50 mm and 3.23 mm, respectively, and the crosshairs width is 0.1-0.2 mm. The above-mentioned apertures can be used interchangeably according to research needs.

[0064] The first cemented imaging lens 11 has an aperture of 25.4 to 50.8 mm and a focal length range of 100 to 200 mm, and is used to form a primary focus.

[0065] The third plane reflector 12 has an aperture of 25.4 to 50.8 mm and is used for folding the optical path.

[0066] The second cemented collimating lens 13 has an aperture of 25.4 to 50.8 mm and a focal length range of 200 to 400 mm, and is used to scale the size of the simulated pupil of the telescope.

[0067] The second cemented imaging lens 14 has an aperture of 25.4 to 50.8 mm and a focal length range of 200 to 400 mm, and is used to form a secondary focus and an F number that matches the ultra-high contrast imaging instrument.

[0068] The first deformable mirror controller 15 and the second deformable mirror controller 16 have 97 drive signal channels, a response time of <10 μs, and a power consumption of <150 W, and respectively drive the actuator displacements of the first deformable mirror 7 and the second deformable mirror 9 .

[0069] In summary, the present invention discloses a telescope system simulation method and device for testing ultra-high-contrast imagers. The simulation device includes a laser-driven white light source, an optical fiber, a microscope objective lens, a pinhole, a first cemented collimating lens, a first plane reflector, a first deformable mirror, a second plane reflector, a second deformable mirror, a telescope pupil simulation aperture, a first cemented imaging lens, a third plane reflector, a second cemented collimating lens, a second cemented imaging lens, a first deformable mirror controller, and a second deformable mirror controller. The present invention can simulate the dynamic perturbations of the incident light wavefront caused by upper- and lower-level atmospheric turbulence during ground-based astronomical telescope imaging observations, allowing for more realistic performance testing of ultra-high-contrast imaging instruments. It can also simulate the pupil shape and position of an astronomical telescope, enabling accurate estimation of the imaging contrast of the ultra-high-contrast imaging instrument when using different telescopes. The device is specifically optimized for the docking datum and pupil optical transfer requirements of the ultra-high-contrast imaging instrument, facilitating docking testing of the ultra-high-contrast imaging instrument.

[0070] This embodiment is only illustrated by taking the white light source with a spectral range of 350 to 2500 nm, the actuators of the first deformable mirror and the second deformable mirror as 97 units, and simulating the pupils of four typical 2-4 meter-class aperture single-primary mirror astronomical telescopes at home and abroad as examples. However, it is easy for those skilled in the art to understand that the above is only a preferred embodiment of the present invention and is not intended to limit the present invention. Any modifications, equivalent substitutions and improvements made within the spirit and principles of the present invention should be included in the scope of protection of the present invention.

Claims

1. A telescope system simulation method for ultra-high contrast imager testing, characterized in that: The steps include: Step 1: Generate a point source of white light to simulate incident starlight; Step 2: collimate the white light point source into parallel light, and then reflect the parallel light onto the first deformable mirror; Step 3: The light is reflected by the first deformable mirror and then incident on the second deformable mirror; Step 4: Use a computer to read the phase screen images of simulated upper atmospheric turbulence and near-ground atmospheric turbulence respectively; Step 5: Controlling the actuator unit matrices of the first deformable mirror and the second deformable mirror to move row by row or column by column on a phase screen image simulating upper atmospheric turbulence and near-ground atmospheric turbulence, respectively, and establishing a conversion relationship between the pixel values ​​of the phase screen image and the travel amount of the deformable mirror actuator; Step 6: The parallel light with wavefront distortion is reflected by the second deformable mirror and then passes through the telescope pupil simulation aperture, wherein the telescope pupil simulation aperture is used to simulate the pupil shape and pupil position of an astronomical telescope; Step 7: The parallel light containing wavefront distortion and the shape of the telescope's simulated pupil is converged to form a primary focus, and then collimated into parallel light to achieve scaling of the telescope's simulated pupil size; Step 8: The scaled parallel light is converged to form a secondary focus. The ultra-high contrast imaging instrument uses the secondary focus as a docking reference. After the optical transfer according to steps 6 to 8, the telescope simulated pupil is conjugated to the wavefront correction unit by the collimating lens inside the ultra-high contrast imaging instrument.

2. The telescope system simulation method for ultra-high contrast imager testing according to claim 1, characterized in that: In step 3, the first deformable mirror and the second deformable mirror are used to simulate the disturbance effects of high-altitude atmospheric turbulence and near-ground atmospheric turbulence, respectively.

3. The telescope system simulation method for ultra-high contrast imager testing according to claim 1, characterized in that: In step 4, the actuator unit matrices of the first deformable mirror and the second deformable mirror are respectively mapped to the phase screen image matrix simulating high-altitude atmospheric turbulence and near-ground atmospheric turbulence. There is no requirement for the initial alignment position between the two matrix elements and they can be any position.

4. The telescope system simulation method for ultra-high contrast imager testing according to claim 1, characterized in that: In step 5, the stroke amounts of the actuators of the first deformable mirror and the second deformable mirror are obtained by converting the numerical values ​​of the phase screen image pixels simulating high-altitude atmospheric turbulence and near-ground atmospheric turbulence respectively, and then the real-time driving voltage signals of the actuators of the first deformable mirror and the second deformable mirror are obtained respectively based on the relationship between the input control signal range of the first deformable mirror and the second deformable mirror and their maximum stroke amounts.

5. The telescope system simulation method for ultra-high contrast imager testing according to claim 1, characterized in that: In step 6, when simulating the pupil of an astronomical telescope with a single primary mirror, the telescope pupil simulation aperture is realized by opening up part of the area on an opaque flat plate, including an outer circle, an inner circle and a crosshair, the outer circle and the inner circle are concentric, the center of the crosshair coincides with the center of the circle and symmetrically passes through the outer circle and the inner circle; wherein, the area between the outer circle and the inner circle is translucent, simulating the light-transmitting area of ​​the telescope primary mirror; the inner circle is opaque, simulating the obstruction of the telescope secondary mirror projected on the primary mirror; the crosshairs are opaque, simulating the obstruction of the telescope secondary mirror support rib projected on the primary mirror.

6. A device for implementing the method according to any one of claims 1 to 5, characterized in that: The device includes a laser-driven white light source, an optical fiber, a microscope objective lens, a pinhole, a first glued collimating lens, a first plane reflector, a first deformable mirror, a second plane reflector, a second deformable mirror, a telescope pupil simulation aperture, a first glued imaging lens, a third plane reflector, a second glued collimating lens, and a second glued imaging lens, which are arranged in sequence along the light path. The device also includes a first deformable mirror controller and a second deformable mirror controller connected to a computer, and the first deformable mirror controller and the second deformable mirror controller respectively drive the displacement of the actuators of the first deformable mirror and the second deformable mirror.

7. The device according to claim 6, characterized in that After being output by optical fiber coupling, the laser-driven white light source is converged by the microscope objective lens onto a pinhole to generate a white light point source, simulating incident starlight. The first cemented collimating lens collimates the white light point source into parallel light, which is then reflected by the first plane reflector to the first deformable mirror. The first deformable mirror reflects the light to the second plane reflector and then to the second deformable mirror. The first deformable mirror and the second deformable mirror are respectively used to simulate the disturbance effects of high-altitude atmospheric turbulence and near-ground atmospheric turbulence. The parallel light with wavefront distortion passes through the telescope pupil simulation aperture, which is used to simulate the pupil shape and pupil position of an astronomical telescope. The parallel light with wavefront distortion and the simulated telescope pupil shape is converged by the first cemented imaging lens to form a primary focus, and then reflected by the third plane reflector and collimated by the second cemented collimating lens into parallel light, thereby scaling the size of the simulated telescope pupil. The scaled parallel light is converged by the second cemented imaging lens to form a secondary focus. The ultra-high contrast imaging instrument uses the secondary focus as a docking reference.

8. The device according to claim 6, characterized in that The telescope pupil simulation aperture is located at a position of one focal length of the first cemented imaging lens, the distance between the second cemented collimating lens and the second cemented imaging lens is equal to the sum of the focal lengths of the two, and the F number of the secondary focus is less than or equal to the F number of the collimating lens inside the ultra-high contrast imaging instrument, wherein the F number of the secondary focus is, F number = f R2 / d pupil_mag , where f R2 is the focal length of the second cemented imaging lens, d pupil_mag It is the scaled telescope simulated pupil size. The secondary focus is located at a position one focal length in front of the collimating lens inside the ultra-high contrast imaging instrument. The wavefront correction unit inside the ultra-high contrast imaging instrument is located at a position one focal length behind its collimating lens. The telescope simulated pupil is finally conjugated to the wavefront correction unit.

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