CN105466576B - Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence - Google Patents

Abstract

The invention provides a device and method for synchronous measurement of atmospheric turbulence height and angle non-uniform wave front error, using two independent high-order large-field Hartmann sensors in a high-order large-field double Hartmann sensor module , the signal generator is used for synchronous triggering and synchronous acquisition of the imaging sub-spot array images of the binary star system and artificial beacons, and the high-speed tilting mirror is used to correct the wavefront error tilt term that cannot be detected by artificial beacons in real time; finally through the wavefront The restoration algorithm respectively obtains the restoration wavefronts between the two natural beacons and the artificial beacons in the binary star system, and calculates the difference between the restoration wavefronts among the three to obtain the height and angle non-equal halo wavefront error results and the height and angle at the same moment. Correlation between angular non-uniform wavefront errors. The invention can be adapted to the measurement under different atmospheric turbulence conditions, has a simple measurement principle, and provides important reference significance for the design and demonstration of the artificial beacon adaptive optical system in the astronomical telescope.

Description

A device for synchronous measurement of atmospheric turbulence height and angle anequal wave front error and method

technical field

The invention belongs to the technical field of optical information measurement, and relates to a device and method for synchronously measuring the wave front error of atmospheric turbulent height non-isohalosis and angle non-equal halo, specifically the atmospheric turbulence height based on double large-field Hartmann sensors Device and method for synchronous measurement of non-uniform and angular non-uniform wavefront errors.

Background technique

Atmospheric turbulence caused by factors such as solar radiation causes random fluctuations in the refractive index of the atmosphere, which affects the performance of the optical system of ground-based astronomical telescopes. Adaptive optics can make corresponding corrections to the target light wavefront. However, astronomical adaptive optics systems for real-time correction of atmospheric turbulence usually require one or more beacons with a sufficient number for real-time wavefront detection. Beacons can use natural stars, that is, the target itself or nearby stars, which are called natural beacons; they can also be artificially stimulated by lasers, which are called artificial beacons. There are two ways to produce artificial beacons: one is to use gas molecules in the atmosphere to excite them with laser light to produce Rayleigh scattering, which is called Rayleigh beacons. Due to the limitation of gas distribution in the atmosphere, its height generally does not exceed 30km; The other is to use sodium atoms in the middle layer of the atmosphere to excite them with sodium yellow light to produce resonance scattering, which is called sodium beacons, and its height, that is, the height of the sodium layer, is generally between 90-120km.

However, in the actual use of the beacon, due to the difference in height and angular distance between the beacon and the observed target, the paths taken by the beacon light to reach the surface of the telescope and the path of the target light to reach the surface of the telescope are also different. , the resulting difference between the wavefront disturbance detected by the beacon light and the wavefront disturbance of the actually observed target is called the non-uniform wavefront error. There are two types of non-uniform wavefront errors, one is caused by the different heights between the beacon and the observed target, which is called height non-isohalo (or focus non-isohalo) wavefront error; the other is caused by the beacon Caused by the angular distance from the observed target, it is called angular non-uniform wavefront error. Usually, when man-made beacons are used for detection, due to their limited height and the angular distance between them and the observed target in use, their non-equal halo error is composed of height non-iso halo error and angle non-iso halo error. It is very important for the performance analysis and optimal design of astronomical adaptive optics systems to understand and master the height non-isohalo error and angle non-isohalo error in artificial beacon detection respectively.

At present, there are mainly two methods for theoretical analysis of the non-isohalo error of beacon detection. One is to use Merlin transform combined with transverse spectral filtering method for analytical analysis, and the other is to use the atmospheric phase screen for numerical solution. However, the theoretical analysis is based on certain atmospheric environmental conditions, and the atmospheric model, calculation method, and boundary conditions used will affect the accuracy of the actual results. For the experimental measurement of the non-isohalo error of beacon wavefront detection, currently there is only a comprehensive measurement of the non-isohalo error of the height and the non-isohalo of the angle. Errors are distinguished and reported for simultaneous measurements.

Contents of the invention

The problem to be solved by the present invention is to overcome the deficiencies of the prior art and combine artificial beacon technology to provide a device and method for synchronous measurement of atmospheric turbulence height and angle non-uniform wave front error. Simultaneous measurement of non-iso-halo error, non-iso-halo error of angle, and combined non-iso-halo error of height non-iso-halo error and angle non-iso-halo error, and gives both height non-iso halo error and angle non-iso halo error The influence on the comprehensive non-isohalo error and the correlation between the two. At the same time, the tilt mirror is controlled in combination with the tilt signal in the wavefront detection, which reduces the influence of the low-order wavefront phase difference that cannot be detected by artificial beacons, and further reduces the measurement error in the experiment.

In order to achieve the above object, the technical solution adopted in the present invention is: a device for synchronously measuring the height and angle of the atmospheric turbulent wave front error, including a telescope (1), a beam reduction module (2), a high-speed tilting mirror (3 ), beam splitter (4), low-order Hartmann sensor module (5); it is characterized in that: it also includes a high-order large field of view double Hartmann sensor module (6), and the high-order large field of view double Hartmann sensor module The Mann sensor module (6) consists of two independent first high-order large field of view Hartmann sensors (7) and second high-order large field of view Hartmann sensors (8), as well as the second beam splitter (27) and Mirror (28) is made up; Wherein, the first high-order Hartmann sensor (7) is made up of the first optical filter (15), the first matching lens group (16), the first space diaphragm (17) , the first high-order microlens array group (18), the first CCD camera (19), the first data acquisition computer (20); the second high-order Hartmann sensor with large field of view (8) is composed of the second filter sheet (21), the second matching lens group (22), the second space diaphragm (23), the second high-order microlens array group (24), the second CCD camera (25), the second data acquisition computer (26 ) composition; the second beamsplitter (27) reflects the return light of the binary star system composed of natural beacon A and natural beacon B into the first high-order large field of view Hartmann sensor (7), and passes through the first filter ( 15) Filter out artificial beacon signals, narrow the beam to a suitable aperture by the first matching lens group (16), filter out other spatial light effects by the first spatial diaphragm (17), and pass through the first high-order microlens array group After (18), the light spot sub-array image obtained is received by the first CCD camera (19) and collected by the first data acquisition computer (20); ) is reflected into the second high-order large field of view Hartmann sensor (8), the signal of the binary star system is filtered out by the second filter (21), and the beam is narrowed to a suitable aperture by the second matching lens group (22). The second spatial aperture (23) filters out other spatial light influences, and after the second high-order microlens array group (24), the light spot sub-array image is received by the second CCD camera (25) and is received by the second data acquisition computer ( 26) Acquisition: The two CCD cameras (19, 25) are synchronously triggered by the signal generator (9), and the image data are recorded through their respective data acquisition computers (20, 26).

The described device for synchronous measurement of atmospheric turbulence height and angle non-equal wavefront error is characterized in that: the low-order Hartmann sensor module (5) consists of a low-order matching lens group (11), a low-order micro Composed of a lens array group (12), a low-order CCD camera (13), and a wavefront processing computer (14), the return light of the binary star system transmitted by the first beam splitter (4) is narrowed by the low-order matching lens group (11) to Appropriate caliber, the imaging light spot sub-array image obtained after imaging by the low-order microlens array group (12) is collected by the low-order CCD camera (13), and the oblique component is extracted after the wavefront restoration calculation by the wavefront processing computer (14). To control the high-speed tilting mirror (3).

A method for synchronously measuring wave front errors of atmospheric turbulence height and angle non-isohalo, which is characterized in that the simultaneous measurement of atmospheric turbulence height non-isohalo and angle non-isohalo wave front errors needs to be carried out according to the following specific steps:

(a) Select a binary star system with an angular distance within 10 arcseconds, the binary star system is composed of natural beacon A and natural beacon B, adjust the optical axis of the telescope (1) to the center of the binary star system, and adjust the laser emission of the artificial beacon The optical axis of the telescope (10) makes the artificial beacon point to the natural beacon A position in the binary star system;

(b) The telescope (1) receives the return light from the double star system composed of natural beacon A and natural beacon B and the artificial beacon, and is reflected to the first beam splitter by the high-speed tilting mirror (3) after passing through the beam reduction module (2) (4), part of the energy back light is transmitted into the low-order Hartmann sensor module (5), and the other part of the energy back light is reflected into the high-order large field of view double Hartmann sensor module (6);

(c) The return light transmitted into the low-order Hartmann sensor module (5) is narrowed to a suitable aperture by the low-order matching lens group (11), and the imaging light spot obtained after imaging by the low-order microlens array group (12) The array image is collected by a low-order CCD camera (13) and collected by a wavefront processing computer (14). The sub-spot array image of the natural beacon A is extracted from the collected imaging sub-spot array image of the binary star system, and is passed through the wavefront The slope component of the wavefront disturbance calculated by the restoration algorithm is used to control the high-speed tilting mirror (3) to improve system stability and reduce back-end measurement errors;

(d) The return light entering the high-order large field of view dual Hartmann sensor module (6) is reflected by the second beam splitter (27), and then the return light of the double star system composed of natural beacon A and natural beacon B is reflected into the first A high-order Hartmann sensor (7) with a large field of view filters artificial beacon signals through the first optical filter (15), and narrows the beam to a suitable aperture by the first matching lens group (16). The aperture (17) filters out the influence of other spatial light, and after passing through the first high-order microlens array group (18), the light spot sub-array image is received by the first CCD camera (19) and collected by the first data acquisition computer (20) After the second beam splitter (27) is transmitted, the man-made beacon is returned to the light and is reflected by the reflector (28) and enters the second high-order large field of view Hartmann sensor (8), and passes through the second optical filter (21 ) to filter out the binary star system signal, and narrow the beam to a suitable aperture by the second matching lens group (22), filter out other space light effects by the second space diaphragm (23), and pass through the second high-order microlens array group (24 ) to obtain the light spot sub-array image is received by the second CCD camera (25) and collected by the second data acquisition computer (26); the two-way CCD cameras (19, 25) are triggered synchronously by the signal generator (9), and respectively Image data is recorded by respective data acquisition computers (20, 26).

(e) After the sub-spot array images of the collected binary star system are extracted, the sub-spot array images of natural beacon A and natural beacon B are obtained respectively; Restoring the sub-spot array images of the artificial beacons and the artificial beacons to obtain the restoration wavefront results and Zernike coefficients of each order of the three, and comparing the wavefront results of the natural beacon A and the artificial beacons to obtain a highly non-uniform halo wave Comparing the wave measurement results of natural beacon A and natural beacon B, the angle non-uniform wave front error is obtained; comparing the wave front detection results of natural beacon B and artificial beacons, the result is a combination of height and angle Synthetic wave front non-equal halo error; thus, the synchronous measurement of atmospheric turbulence height and angle non-equal halo wave front error and the measurement of the correlation between height and angle non-iso halo wave front error are completed.

Compared with the prior art, the present invention has the following advantages:

(1) the present invention is to the device and method of synchronous measurement of atmospheric turbulence height non-equal halo and angle non-equal halo wave front error, has utilized the characteristic that only has angle non-equal halo wave front error between binary star system; Simultaneously, has utilized for pointing The same man-made beacons and natural beacons only have the characteristic of non-equal halo wavefront error; by comparing the wavefront results of two natural beacons and artificial beacons in a binary star system, the simultaneous estimation of height and angle non-equal halos can be achieved. Halo front error synchronization measurement purposes.

(2) The measurement principle of the present invention is clear, the measurement device is simple, and the measurement is small.

Description of drawings

Fig. 1 is the structure schematic diagram of the synchronous measurement device for atmospheric turbulence height and angle anequal wave front error of the present invention;

Fig. 2 is the structural representation of the low-order Hartmann sensor module in the synchronous measurement device for atmospheric turbulence height and angle non-equal halo wavefront error of the present invention;

Fig. 3 is a structural schematic diagram of a high-order large field of view double Hartmann sensor module in the synchronous measurement device for atmospheric turbulence height and angle non-uniform wavefront error of the present invention;

Fig. 4 is a structural schematic diagram of a wavefront sensor in a high-order large field of view double Hartmann sensor module in the high-order large field of view dual Hartmann sensor module of the present invention to the atmospheric turbulence height and angle non-equal halo wavefront error synchronization measurement device;

Fig. 5 is a structural schematic diagram of another high-order Hartmann in the high-order large field of view double Hartmann sensor module in the synchronous measurement device for atmospheric turbulence height and angle non-uniform wavefront error of the present invention;

In the figure: 1. Telescope 2. Beam reduction module 3. High-speed tilting mirror 4. First beam splitter 5. Low-order Hartmann sensor module 6. High-order large field of view double Hartmann sensor module 7. First high-order Large field of view Hartmann sensor 8. Second high-order large field of view Hartmann sensor 9. Signal generator 10. Artificial beacon laser transmitting telescope 11. Low-order matching lens group 12. Low-order microlens array group 13. Low-order CCD camera 14. Wavefront processing computer 15. First optical filter 16. First matching lens group 17. First space diaphragm 18. First high-order microlens array group 19. First CCD camera 20. The first A data acquisition computer 21. The second optical filter 22. The second matching lens group 23. The second space diaphragm 24. The second high-order microlens array group 25. The second CCD camera 26. The second data acquisition computer 27. Second beam splitter 28. Mirror

Detailed ways

The present invention will be further described below in conjunction with the accompanying drawings and specific embodiments.

Example 1:

Fig. 1 is a schematic structural view of the device for synchronously measuring the wavefront error of atmospheric turbulence height non-isohalation and angle non-isohalation according to the present invention, including a telescope 1, a beam reduction module 2, a high-speed tilting mirror 3, a first beam splitter 4, a low High-order Hartmann sensor module 5, high-order large field of view double Hartmann sensor module 6, and other supporting equipment such as signal generator 9 and artificial beacon laser emitting telescope 10.

Fig. 2 is a schematic structural view of the low-order Hartmann sensor module 5 in the synchronous measurement device for atmospheric turbulence height and angle non-uniform wavefront error disclosed by the present invention, consisting of a low-order matching lens group 11 and a low-order microlens array group 12 , a low-order CCD camera 13, and a wavefront processing computer 14.

Fig. 3 is a structural schematic diagram of a high-order large field of view double Hartmann sensor module 6 in a synchronous measurement device for atmospheric turbulence height and angle non-uniform wavefront error disclosed by the present invention, which consists of two independent first high-order large field of view sensors. Hartmann sensor 7, the second high-order large field of view Hartmann sensor 8, the second beam splitter 27, and reflector 28; wherein, Fig. 4 is the structure of the first high-order large field of view Hartmann sensor 7 Schematic diagram, composed of the first optical filter 15, the first matching lens group 16, the first spatial diaphragm 17, the first high-order microlens array group 18, the first CCD camera 19, and the first data acquisition computer 20; FIG. 5 It is a structural schematic diagram of the second high-order large field of view Hartmann sensor 8, which consists of a second optical filter 21, a second matching lens group 22, a second space diaphragm 23, a second high-order microlens array group 24, and a second high-order microlens array group 24. Two CCD cameras 25 and a second data acquisition computer 26 form.

In the present invention, the method for synchronous measurement of atmospheric turbulent height and angle non-uniform wave front error is as follows:

(a) Select a double star system, which is made up of natural beacon A and natural beacon B, adjust the optical axis of the telescope (1) to the center of the double star system, adjust the optical axis of the artificial beacon laser emitting telescope (10) so that The artificial beacon points to the position of natural beacon A in the binary star system;

(b) The telescope (1) receives the return light from the double star system composed of natural beacon A and natural beacon B and the artificial beacon, and is reflected to the first beam splitter by the high-speed tilting mirror (3) after passing through the beam reduction module (2) (4), part of the energy back light is transmitted into the low-order Hartmann sensor module (5), and the other part of the energy back light is reflected into the high-order large field of view double Hartmann sensor module (6);

(c) The return light transmitted into the low-order Hartmann sensor module (5) is narrowed to a suitable aperture by the low-order matching lens group (11), and the imaging light spot obtained after imaging by the low-order microlens array group (12) The array image is collected by a low-order CCD camera (13), collected by a wavefront processing computer (14), and the sub-spot array image of the natural beacon A is extracted from the collected imaging sub-spot array image of the binary star system, and the sub-spot array image of each sub-aperture is calculated. The drift of the center of the upper spot in the X and Y directions can be used to calculate the average slope of the wavefront in the two directions within the range of each sub-aperture:

Among them, λ is the center wavelength of the imaging band, f is the focal length of the microlens, I _i is the signal received by pixel i, Xi _and Y _i are the coordinates of the i-th pixel, Φ(x, y) is the wavefront to be calculated , (X _C , Y _C ) is the coordinates of the spot centroid, (G _X , G _Y ) is the average slope of the wavefront, and S is the sub-aperture area;

After obtaining the sub-aperture slope data, the coefficients of Zernike aberrations of each order are obtained through the mode restoration algorithm, so that the measured wavefront data can be directly superimposed in the circular domain. Assuming that the input signal _aj is added to the j-th order Zernike aberration coefficient, the average wavefront slope in the sub-aperture of the Hartmann sensor is:

j = 1, 2, 3, 4, 5...

Where Z _j (x, y) is the jth order Zernike function, t is the Zernike order, and S is the normalized area of the circle domain. The slope of the sub-aperture is linearly related to the Zernike coefficient, both of which satisfy the superposition principle, so the above formula can be written in the form of a matrix:

G＝ _ZxyA

Z _xy is the corresponding matrix of the Zernike aberration to the slope of the Hartmann sensor, which can be calculated; G is the measured value of the wavefront phase difference slope, so the Zernike coefficient can be obtained:

A＝Z ⁺ _xyG

in, for The generalized inverse; in this way, the coefficient A of each order Zernike aberration is obtained. Among them, A ₂ and A ₃ are the tilt items of the wavefront phase difference, and the results of these two items are used to control the high-speed tilt mirror (3), so as to improve the system stability and reduce the back-end measurement error;

(d) The return light entering the high-order large field of view dual Hartmann sensor module (6) is reflected by the second beam splitter (27), and then the return light of the double star system composed of natural beacon A and natural beacon B is reflected into the first A high-order Hartmann sensor (7) with a large field of view filters artificial beacon signals through the first optical filter (15), and narrows the beam to a suitable aperture by the first matching lens group (16). The aperture (17) filters out the influence of other spatial light, and after passing through the first high-order microlens array group (18), the light spot sub-array image is received by the first CCD camera (19) and collected by the first data acquisition computer (20) After the second beam splitter (27) is transmitted, the man-made beacon is returned to the light and is reflected by the reflector (28) and enters the second high-order large field of view Hartmann sensor (8), and passes through the second optical filter (21 ) to filter out the binary star system signal, and narrow the beam to a suitable aperture by the second matching lens group (22), filter out other space light effects by the second space diaphragm (23), and pass through the second high-order microlens array group (24 ) to obtain the light spot sub-array image is received by the second CCD camera (25) and collected by the second data acquisition computer (26); the two-way CCD cameras (19, 25) are triggered synchronously by the signal generator (9), and respectively Image data is recorded by respective data acquisition computers (20, 26).

(e) After the sub-spot array images of the collected binary star system are extracted, the sub-spot array images of natural beacon A and natural beacon B are respectively obtained; for the extracted natural beacon A, natural beacon B and artificial beacon The target sub-spot array image is respectively subjected to wavefront restoration calculation, and the calculation method is as follows:

Calculate the drift of the center of the spot on each sub-aperture in the X and Y directions for the sub-spot array image, and the average slope of the wavefront in the two directions within the range of each sub-aperture can be obtained:

Among them, λ is the center wavelength of the imaging band, f is the focal length of the microlens, I _i is the signal received by pixel i, Xi _and Y _i are the coordinates of the i-th pixel, Φ(x, y) is the wavefront to be calculated , (X _C , Y _C ) is the coordinates of the spot centroid, (G _X , G _Y ) is the average slope of the wavefront, and S is the sub-aperture area;

After obtaining the sub-aperture slope data, the coefficients of Zernike aberrations of each order are obtained through the mode restoration algorithm, so that the measured wavefront data can be directly superimposed in the circular domain. Assuming that the input signal _aj is added to the j-th order Zernike aberration coefficient, the average wavefront slope in the sub-aperture of the Hartmann sensor is:

j = 1, 2, 3, 4, 5...

Among them, Z _j (x, y) is the jth order Zernike function, t is the Zernike order, S is the normalized area of the circular domain; the slope of the sub-aperture is linearly related to the Zernike coefficient, and both satisfy the principle of superposition, so the above formula It can be written in matrix form:

G＝ _ZxyA

Z _xy is the corresponding matrix of the Zernike aberration to the slope of the Hartmann sensor, which can be calculated; G is the measured value of the wavefront phase difference slope, so the Zernike coefficient can be obtained:

A＝Z ⁺ _xyG

in, for The generalized inverse of . In this way, the coefficient A of each order of Zernike aberration is obtained. The wavefront Φ(x, y) to be measured is obtained by the following expression:

In the formula, A _j is the coefficient of the j-th Zernike aberration, and Z _j (x, y) is the j-th Zernike polynomial.

Finally, the wavefront restoration results of natural beacon A, natural beacon B, and artificial beacon and the Zernike coefficients of each order are obtained; comparing the wavefront results of natural beacon A and artificial beacon results in a highly non-uniform wavefront error ; Comparing the wave measurement results of natural beacon A and natural beacon B, the angle non-uniform wavefront error is obtained; comparing the wavefront detection results of natural beacon B and artificial beacons, the result is a composite wave combining height and angle Front non-uniform error; thus completed the simultaneous measurement of atmospheric turbulence height and angle non-uniform wave front error and the measurement of the correlation between height and angle non-uniform wave front error.

Claims (3)

1. A synchronous measurement device for height and angle non-isoplanatic wavefront errors of atmospheric turbulence comprises a telescope (1), a beam shrinking module (2), a high-speed tilting mirror (3), a first spectroscope (4) and a low-order Hartmann sensor module (5); the method is characterized in that: the system also comprises a high-order large-view-field double-Hartmann sensor module (6), wherein the high-order large-view-field double-Hartmann sensor module (6) consists of a first high-order large-view-field Hartmann sensor (7) for respectively extracting a natural beacon A signal and a natural beacon B signal, a second high-order large-view-field Hartmann sensor (8) for measuring an artificial beacon signal, a second beam splitter (27) and a reflector (28); the first high-order large-field Hartmann sensor (7) consists of a first optical filter (15), a first matching lens group (16), a first space diaphragm (17), a first high-order micro lens array group (18), a first CCD camera (19) and a first data acquisition computer (20); the second high-order large-field Hartmann sensor (8) consists of a second optical filter (21), a second matching lens group (22), a second space diaphragm (23), a second high-order micro lens array group (24), a second CCD camera (25) and a second data acquisition computer (26); a second spectroscope (27) reflects return light of a double-star system consisting of a natural beacon A and a natural beacon B to enter a first high-order large-field Hartmann sensor (7), artificial beacon signals are filtered by a first optical filter (15), the return light is contracted to a proper aperture by a first matching lens group (16), other spatial light influences are filtered by a first spatial diaphragm (17), and a light spot subarray image obtained after passing through a first high-order microlens array group (18) is received by a first CCD camera (19) and is collected by a first data collection computer (20); the second spectroscope (27) transmits return light of the artificial beacon and reflects the return light by the reflector (28) to enter a second high-order large-field-of-view Hartmann sensor (8), a double-star system signal is filtered by a second optical filter (21), the return light is condensed to a proper caliber by a second matching lens group (22), other space light influence is filtered by a second space diaphragm (23), a light spot sub-array image is obtained after passing through a second high-order micro lens array group (24), and the light spot sub-array image is received by a second CCD camera (25) and is collected by a second data collection computer (26); two CCD cameras (19, 25) are synchronously triggered by a signal generator (9), double-star image data are recorded by a first data acquisition computer (20), artificial beacon image data are recorded by a second data acquisition computer (26), restored wavefronts between two natural beacons and the artificial beacons in the double-star system are respectively obtained through a wavefront restoration algorithm, and the height and angle non-isoplanar wavefront error result and the correlation between the height and angle non-isoplanar wavefront errors at the same moment are obtained through calculation of restored wavefront differences among the three.

2. The device for synchronously measuring the wavefront error with the non-isohalo to the height and the angle of the atmospheric turbulence as recited in claim 1, wherein: the low-order Hartmann sensor module (5) is composed of a low-order matching lens group (11), a low-order micro-lens array group (12), a low-order CCD camera (13) and a wave front processing computer (14), wherein double-star system return light transmitted by the first spectroscope (4) is shrunk to a proper caliber by the low-order matching lens group (11), an imaging light spot sub-array image obtained after imaging by the low-order micro-lens array group (12) is collected by the low-order CCD camera (13), and an inclined component is extracted through the wave front processing computer (14) after wave front restoration calculation to control the high-speed tilting mirror (3).

3. A synchronous measurement method for the height and angle non-isohalo wavefront error of atmospheric turbulence is characterized by comprising the following implementation steps:

(a) selecting a double-star system with an angular interval within 10 arc seconds, wherein the double-star system consists of a natural beacon A and a natural beacon B, adjusting the optical axis of a telescope (1) to the central position of the double-star system, and adjusting the optical axis of an artificial beacon laser emission telescope (10) to enable an artificial beacon to point to the position of the natural beacon A in the double-star system;

(b) the telescope (1) receives return light of a double-star system consisting of a natural beacon A and a natural beacon B and an artificial beacon, the return light passes through the beam shrinking module (2) and then is reflected to the first spectroscope (4) by the high-speed inclined mirror (3), return light of a part of energy is transmitted to enter the low-order Hartmann sensor module (5), and return light of the other part of energy is reflected to enter the high-order large-view-field double-Hartmann sensor module (6);

(c) the return light transmitted into the low-order Hartmann sensor module (5) is shrunk to a proper caliber by a low-order matching lens group (11), an imaging light spot sub-array image obtained after imaging by a low-order micro-lens array group (12) is collected by a low-order CCD camera (13), the imaging light spot sub-array image is collected by a wavefront processing computer (14), a sub-light spot array image of a natural beacon A is extracted from the collected imaging sub-light spot array image of the double-star system, an inclination component of wavefront disturbance is calculated by a wavefront restoration algorithm, and the inclination component is used for controlling the high-speed inclined mirror (3) so as to improve the system stability and reduce the rear-end measurement error;

(d) the return light entering the high-order large-view-field double-Hartmann sensor module (6) is reflected by a second spectroscope (27), then the return light of a double-star system consisting of a natural beacon A and a natural beacon B is reflected to enter a first high-order large-view-field Hartmann sensor (7), an artificial beacon signal is filtered by a first optical filter (15), the artificial beacon signal is contracted to a proper aperture by a first matching lens group (16), other spatial light influence is filtered by a first spatial diaphragm (17), and a light spot subarray image obtained after passing through a first high-order micro lens array group (18) is received by a first CCD camera (19) and is collected by a first data collection computer (20); after being transmitted by a second spectroscope (27), the return light of the artificial beacon is transmitted and reflected by a reflector (28) to enter a second high-order large-field Hartmann sensor (8), a double-star system signal is filtered by a second optical filter (21), the signal is condensed to a proper aperture by a second matching lens group (22), other spatial light influence is filtered by a second spatial diaphragm (23), and a light spot subarray image obtained after passing through a second high-order micro lens array group (24) is received by a second CCD camera (25) and is collected by a second data collection computer (26); the two CCD cameras (19, 25) are synchronously triggered by a signal generator (9) and respectively record image data through respective data acquisition computers (20, 26);

(e) extracting the collected sub light spot array images of the double-satellite system to respectively obtain sub light spot array images of a natural beacon A and a natural beacon B; respectively carrying out restoration calculation on sub-light spot array images of the natural beacon A, the natural beacon B and the artificial beacon through a wavefront restoration algorithm to obtain restoration wavefront results of the natural beacon A, the natural beacon B and the artificial beacon and Zernike coefficients of all orders, and comparing the wavefront results of the natural beacon A and the artificial beacon to obtain a wavefront error with non-uniform height; the wave measurement results of the natural beacon A and the natural beacon B are compared to obtain the wave front error with the non-equal halo angle; comparing the wavefront detection results of the natural beacon B and the artificial beacon to obtain a comprehensive wavefront non-isoplanatic error combined with the height and the angle; therefore, synchronous measurement of the height and angle non-isohalo wavefront errors of the atmospheric turbulence and measurement of the correlation between the height and angle non-isohalo wavefront errors are completed.