CN105466576B - Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence - Google Patents
Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence Download PDFInfo
- Publication number
- CN105466576B CN105466576B CN201511028343.XA CN201511028343A CN105466576B CN 105466576 B CN105466576 B CN 105466576B CN 201511028343 A CN201511028343 A CN 201511028343A CN 105466576 B CN105466576 B CN 105466576B
- Authority
- CN
- China
- Prior art keywords
- beacon
- order
- wavefront
- double
- natural
- Prior art date
- Legal status (The legal status is an assumption and is not a legal conclusion. Google has not performed a legal analysis and makes no representation as to the accuracy of the status listed.)
- Active
Links
- 238000000034 method Methods 0.000 title claims abstract description 16
- 238000005259 measurement Methods 0.000 claims abstract description 30
- 230000003287 optical effect Effects 0.000 claims abstract description 28
- 125000001475 halogen functional group Chemical group 0.000 claims abstract description 21
- 238000003384 imaging method Methods 0.000 claims abstract description 17
- 230000001360 synchronised effect Effects 0.000 claims description 15
- 238000004364 calculation method Methods 0.000 claims description 10
- 238000013480 data collection Methods 0.000 claims description 10
- 238000001514 detection method Methods 0.000 claims description 9
- 238000012545 processing Methods 0.000 claims description 9
- 230000001960 triggered effect Effects 0.000 claims description 5
- 238000000691 measurement method Methods 0.000 claims description 2
- 230000003044 adaptive effect Effects 0.000 abstract description 4
- 238000012937 correction Methods 0.000 abstract description 3
- 238000013461 design Methods 0.000 abstract description 2
- 238000010586 diagram Methods 0.000 description 10
- 230000004075 alteration Effects 0.000 description 9
- DGAQECJNVWCQMB-PUAWFVPOSA-M Ilexoside XXIX Chemical compound C[C@@H]1CC[C@@]2(CC[C@@]3(C(=CC[C@H]4[C@]3(CC[C@@H]5[C@@]4(CC[C@@H](C5(C)C)OS(=O)(=O)[O-])C)C)[C@@H]2[C@]1(C)O)C)C(=O)O[C@H]6[C@@H]([C@H]([C@@H]([C@H](O6)CO)O)O)O.[Na+] DGAQECJNVWCQMB-PUAWFVPOSA-M 0.000 description 4
- 238000004458 analytical method Methods 0.000 description 4
- 239000011159 matrix material Substances 0.000 description 4
- 229910052708 sodium Inorganic materials 0.000 description 4
- 239000011734 sodium Substances 0.000 description 4
- 230000005284 excitation Effects 0.000 description 2
- 238000011084 recovery Methods 0.000 description 2
- 230000007547 defect Effects 0.000 description 1
- 238000005516 engineering process Methods 0.000 description 1
- 230000007613 environmental effect Effects 0.000 description 1
- 238000002474 experimental method Methods 0.000 description 1
- 238000001914 filtration Methods 0.000 description 1
- 238000005457 optimization Methods 0.000 description 1
- 230000005855 radiation Effects 0.000 description 1
- 125000004436 sodium atom Chemical group 0.000 description 1
- 230000003595 spectral effect Effects 0.000 description 1
Classifications
-
- G—PHYSICS
- G01—MEASURING; TESTING
- G01J—MEASUREMENT OF INTENSITY, VELOCITY, SPECTRAL CONTENT, POLARISATION, PHASE OR PULSE CHARACTERISTICS OF INFRARED, VISIBLE OR ULTRAVIOLET LIGHT; COLORIMETRY; RADIATION PYROMETRY
- G01J9/00—Measuring optical phase difference; Determining degree of coherence; Measuring optical wavelength
Landscapes
- Physics & Mathematics (AREA)
- Spectroscopy & Molecular Physics (AREA)
- General Physics & Mathematics (AREA)
- Telescopes (AREA)
- Length Measuring Devices By Optical Means (AREA)
Abstract
The invention provides a device and a method for synchronously measuring the height and angle non-isohalo wave front error of atmospheric turbulence, which utilize two independent high-order large-view field Hartmann sensors in a high-order large-view field double Hartmann sensor module to synchronously trigger through a signal generator and synchronously acquire imaging sub light spot array images of a double-star system and an artificial beacon, and utilize a high-speed tilting mirror to carry out real-time correction on a wave front error tilting item which can not be detected by the artificial beacon; and finally, respectively obtaining the restored wavefront between the two natural beacons and the artificial beacon in the double-star system through a wavefront restoration algorithm, and calculating the result of the height and angle unequal halo wavefront error at the same moment and the correlation between the height and angle unequal halo wavefront errors through the restored wavefront difference between the two natural beacons and the artificial beacon. The invention can adapt to measurement under different atmospheric turbulence conditions, has 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
Technical Field
The invention belongs to the technical field of optical information measurement, and relates to a device and a method for synchronously measuring the wavefront errors of high non-isohalo and angle non-isohalo of atmospheric turbulence, in particular to a device and a method for synchronously measuring the wavefront errors of high non-isohalo and angle non-isohalo of atmospheric turbulence based on a double-large-field Hartmann sensor.
Background
The atmospheric turbulence caused by factors such as solar radiation causes random fluctuation of the atmospheric refractive index, and influences the performance of an optical system of the ground-based astronomical telescope. Adaptive optics may make corresponding corrections to the target wavefront. However, astronomical adaptive optics for real-time correction of atmospheric turbulence typically require one or more beacons in sufficient quantity for real-time wavefront detection. The beacon can utilize a natural star, namely a measuring star of the target or nearby, and is called as a natural beacon; it may also be generated by artificial excitation with a laser, known as an artificial beacon. There are two methods of generating artificial beacons: one is that gas molecules in the atmosphere are excited by laser to generate Rayleigh scattering, called Rayleigh beacon, and the height of the Rayleigh beacon is limited by the distribution of gas in the atmosphere and generally does not exceed 30 km; the other is to use sodium atoms in the middle layer of the atmosphere to generate resonance scattering by sodium yellow light excitation, which is called sodium beacon, and the height of the sodium beacon, namely the height of the sodium layer, is generally between 90 and 120 km.
However, in the actual use process of the beacon, due to the difference of the height and the angular distance between the beacon and the observed target, the paths through which the beacon light reaches the telescope surface and the target light reaches the telescope surface in the atmosphere are different, and the difference between the wavefront disturbance detected by the beacon light and the wavefront disturbance of the actually observed target, which is caused by the difference, is called as an anisometropic wavefront error. The non-isoplanatic wavefront errors are divided into two types, one type is caused by different heights between a beacon and an observed target, and the height non-isoplanatic (or focusing non-isoplanatic) wavefront error is called; the other is caused by the angular distance between the beacon and the observed target, and is called the angular non-isohalo wavefront error. In general, when a man-made beacon is used for detection, due to the limited height and the angular distance between the man-made beacon and an observed target in use, an unequal halo error of the man-made beacon is composed of a height unequal halo error and an angular unequal halo error. The method is very important for performance analysis and optimization design of the astronomical adaptive optical system to know and master the high non-isoplanatic error and the angle non-isoplanatic error in artificial beacon detection respectively.
At present, there are two main methods for theoretical analysis of beacon detection non-isoplanatic errors, one is analytical analysis by utilizing Mellin transform and combining a transverse spectral filtering method, and the other is numerical solution by utilizing an atmospheric phase screen. However, theoretical analysis is established on the basis of certain atmospheric environmental conditions, and the accuracy between the utilized atmospheric model, calculation method, boundary conditions and the like and actual results is influenced. In the experimental measurement of the beacon wavefront detection non-isoplanatic error, only the comprehensive measurement integrating the height non-isoplanatic error and the angle non-isoplanatic error exists at present, and the report of distinguishing the height non-isoplanatic error and the angle non-isoplanatic error and carrying out synchronous measurement is not seen for a moment.
Disclosure of Invention
The invention provides a device and a method for synchronously measuring the height and angle unequal halo wave front errors of atmospheric turbulence by overcoming the defects of the prior art and combining an artificial beacon technology, the method is suitable for synchronously measuring the height unequal halo errors, the angle unequal halo errors and the comprehensive unequal halo errors combining the height unequal halo errors and the angle unequal halo errors, and gives the influence of the height unequal halo errors and the angle unequal halo errors on the comprehensive unequal halo errors and the correlation between the height unequal halo errors and the angle unequal halo errors. Meanwhile, the tilting mirror is controlled by combining the tilting signal in the wave-front detection, so that the influence of low-order wave-front phase difference which cannot be detected by the artificial beacon is reduced, and the measurement error in the experiment is further reduced.
In order to achieve the purpose, the technical scheme adopted by the invention is as follows: 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 spectroscope (4) and a low-order Hartmann sensor module (5); the method is characterized in that: the high-order double-Hartmann sensor module with the large view field (6) is also included, and the high-order double-Hartmann sensor module with the large view field (6) consists of a first high-order Hartmann sensor with the large view field (7), a second high-order Hartmann sensor with the large view field (8), a second spectroscope (27) and a reflector (28) which are independent in two ways; 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); the two CCD cameras (19, 25) are synchronously triggered by a signal generator (9) and record image data through respective data acquisition computers (20, 26).
The synchronous measurement device for the wavefront error of the atmosphere turbulence with the height and the angle non-isohalo is characterized in that: 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).
A synchronous measurement method for the height and angle non-isoplanatic wavefront error of atmospheric turbulence is characterized in that: the synchronous measurement of the wavefront errors of the atmospheric turbulence with the height unequal halo and the angle unequal halo is realized by the following 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), a wavefront processing computer (14) is used for collecting, 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 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.
Compared with the prior art, the invention has the following advantages:
(1) the invention relates to a device and a method for synchronously measuring the wavefront errors of highly non-isohalo and angularly non-isohalo of atmospheric turbulence, which utilize the characteristic that only angular non-isohalo wavefront errors exist between two-satellite systems; meanwhile, the characteristic that only the height non-isoplanatic wavefront error exists between the artificial beacon and the natural beacon which point at the same direction is utilized; by comparing the wavefront results of two natural beacons and artificial beacons in the double-star system, the aim of synchronously measuring the height and angle non-isohalo wavefront errors is fulfilled.
(2) The invention has clear measuring principle, simple measuring device and small measurement.
Drawings
FIG. 1 is a schematic structural diagram of a wavefront error synchronous measuring device for atmospheric turbulence non-isohalo in height and angle;
FIG. 2 is a schematic structural diagram of a low-order Hartmann sensor module in the device for synchronously measuring the wavefront error of the atmospheric turbulence non-isohalo in height and angle;
FIG. 3 is a schematic structural diagram of a high-order large-field-of-view double Hartmann sensor module in the wavefront error synchronous measurement device for the height and angle non-isohalo of atmospheric turbulence according to the present invention;
FIG. 4 is a schematic structural diagram of a wavefront sensor in a high-order large-field double Hartmann sensor module in the synchronous measurement device for the wavefront error of the atmospheric turbulence height and angle non-isohalo;
FIG. 5 is a schematic structural diagram of another high-order Hartmann in a high-order large-field-of-view double-Hartmann sensor module in the synchronous measurement device for the wavefront error with the non-isohalo height and angle of the atmospheric turbulence;
in the figure: 1. the system comprises a telescope 2, a beam shrinking module 3, a high-speed tilting mirror 4, a first spectroscope 5, a low-order Hartmann sensor module 6, a high-order large-field double Hartmann sensor module 7, a first high-order large-field Hartmann sensor 8, a second high-order large-field Hartmann sensor 9, a signal generator 10, an artificial beacon laser emission telescope 11, a low-order matching lens group 12, a low-order microlens array group 13, a low-order CCD camera 14, a wavefront processing computer 15, a first optical filter 16, a first matching lens group 17, a first spatial diaphragm 18, a first high-order microlens array group 19, a first CCD camera 20, a first data acquisition computer 21, a second optical filter 22, a second matching lens group 23, a second spatial diaphragm 24, a second high-order microlens array group 25, a second CCD camera 26, a second data acquisition computer 27, a second spectroscope 28 and a reflector.
Detailed Description
The invention is further described with reference to the following drawings and detailed description.
Example 1:
fig. 1 is a schematic structural diagram of a wavefront error synchronous measurement device for highly non-isohalo and angularly non-isohalo of atmospheric turbulence, which comprises a telescope 1, a beam shrinking module 2, a high-speed tilting mirror 3, a first spectroscope 4, a low-order hartmann sensor module 5, a high-order large-field double hartmann sensor module 6, and matched equipment such as a signal generator 9 and an artificial beacon laser emission telescope 10.
Fig. 2 is a schematic structural diagram of a low-order hartmann sensor module 5 in the device for synchronously measuring wavefront errors of non-isohalo of atmospheric turbulence height and angle, which is disclosed by the invention, and consists of a low-order matching lens group 11, a low-order microlens array group 12, a low-order CCD camera 13 and a wavefront processing computer 14.
FIG. 3 is a schematic structural diagram of a high-order large-view-field double Hartmann sensor module 6 in the device for synchronously measuring the height and angle non-isohalo wavefront error of the atmospheric turbulence, which is disclosed by the invention and consists of a first high-order large-view-field Hartmann sensor 7, a second high-order large-view-field Hartmann sensor 8, a second beam splitter 27 and a reflector 28 which are independent in two ways; fig. 4 is a schematic structural diagram of the first high-order large-field hartmann sensor 7, which is composed of a first optical filter 15, a first matching lens group 16, a first spatial diaphragm 17, a first high-order microlens array group 18, a first CCD camera 19, and a first data acquisition computer 20; fig. 5 is a schematic structural diagram of the second high-order large-field hartmann sensor 8, which is composed of a second optical filter 21, a second matching lens group 22, a second spatial diaphragm 23, a second high-order microlens array group 24, a second CCD camera 25, and a second data acquisition computer 26.
The invention discloses a method for synchronously measuring the height and angle non-isohalo wavefront errors of atmospheric turbulence, which comprises the following steps:
(a) selecting a double-star system, 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 contracted 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), a wavefront processing computer (14) is used for collecting, 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, the drift of the light spot center on each sub-aperture in the X and Y directions is calculated, and the average slope of the wavefront in each sub-aperture range in two directions can be calculated:
wherein, λ is central wavelength of imaging waveband, f is focal length of microlens, IiIs the signal received by pixel i, Xi，YiIs the coordinate of the ith pixel, phi (X, y) is the wavefront to be calculated, (X)C，YC) Is the coordinate of the centroid of the light spot (G)X，GY) Is the wavefront average slope, S is the subaperture area;
and after the sub-aperture slope data is obtained, the coefficients of Zernike aberration of each order are obtained through a mode recovery algorithm, and thus the measured wave surface data are obtained by directly superposing in a circular domain. Let the input signal ajIs added to the j-th order Zernike aberration coefficients, thereby producing an average wavefront slope magnitude within the sub-aperture of the hartmann sensor of:
j＝1，2，3，4，5……
wherein Zj(x, y) is the Zernike order j function, t is the Zernike order, and S is the normalized area of the circular domain. The slope quantity of the sub-aperture and the Zernike coefficient are in linear relation and both satisfy the superposition principle, so the above formula can be written as a matrix form:
G＝ZxyA
Zxythe matrix corresponding to the slope from the Zernike aberration to the Hartmann sensor can be obtained by calculation; g is the wavefront phase difference slope measurement, so Zernike coefficients can be obtained:
A＝Z+ xyG
wherein,is composed ofThe generalized inverse of (1); thus, the coefficients A of the Zernike aberrations of each order are determined. Wherein A is2、A3The two results are used for controlling the high-speed tilting mirror (3) 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 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 wavefront restoration calculation on the extracted sub-light spot array images of the natural beacon A, the natural beacon B and the artificial beacon, wherein the calculation method comprises the following steps:
calculating the drift of the center of the light spot in each sub-aperture in the X and Y directions for the sub-aperture array image, the average slope of the wavefront in each sub-aperture range in two directions can be found:
wherein, λ is central wavelength of imaging waveband, f is focal length of microlens, IiIs the signal received by pixel i, Xi，YiIs the coordinate of the ith pixel, phi (X, y) is the wavefront to be calculated, (X)C，YC) Is the coordinate of the centroid of the light spot (G)X，GY) Is the wavefront average slope, S is the subaperture area;
and after the sub-aperture slope data is obtained, the coefficients of Zernike aberration of each order are obtained through a mode recovery algorithm, and thus the measured wave surface data are obtained by directly superposing in a circular domain. Let the input signal ajIs added to the j-th order Zernike aberration coefficients, thereby producing an average wavefront slope magnitude within the sub-aperture of the hartmann sensor of:
j＝1，2，3，4，5……
wherein Zj(x, y) is a j-th order function of Zernike, t is the order of Zernike, and S is the normalized area of the circular domain; the slope quantity of the sub-aperture and the Zernike coefficient are in linear relation and both satisfy the superposition principle, so the above formula can be written as a matrix form:
G＝ZxyA
Zxythe matrix corresponding to the slope from the Zernike aberration to the Hartmann sensor can be obtained by calculation; g is the wavefront phase difference slope measurement, so Zernike coefficients can be obtained:
A＝Z+ xyG
wherein,is composed ofThe generalized inverse of (1). Thus, the coefficients A of the Zernike aberrations of each order are determined. The wavefront Φ (x, y) to be measured is obtained by the following expression:
in the formula AjIs a coefficient of Zernike aberration of the j term, Zj(x, y) is a Zernike polynomial of the j-th term.
Finally, obtaining the wavefront restoration results of the natural beacon A, the natural beacon B and the artificial beacon and the Zernike coefficients of all orders; the wavefront results of the natural beacon A and the artificial beacon are compared to obtain a highly non-isohalo wavefront error; 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.
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.
Priority Applications (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN201511028343.XA CN105466576B (en) | 2015-12-31 | 2015-12-31 | Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence |
Applications Claiming Priority (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN201511028343.XA CN105466576B (en) | 2015-12-31 | 2015-12-31 | Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence |
Publications (2)
| Publication Number | Publication Date |
|---|---|
| CN105466576A CN105466576A (en) | 2016-04-06 |
| CN105466576B true CN105466576B (en) | 2018-09-28 |
Family
ID=55604524
Family Applications (1)
| Application Number | Title | Priority Date | Filing Date |
|---|---|---|---|
| CN201511028343.XA Active CN105466576B (en) | 2015-12-31 | 2015-12-31 | Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence |
Country Status (1)
| Country | Link |
|---|---|
| CN (1) | CN105466576B (en) |
Families Citing this family (5)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN106482731B (en) * | 2016-09-29 | 2019-03-15 | 华中光电技术研究所（中国船舶重工集团公司第七一七研究所） | A kind of big visual field survey star sensor and application method of inhibition atmospheric turbulence effect on daytime |
| GB201805275D0 (en) * | 2018-03-29 | 2018-05-16 | Archangel Lightworks Ltd | Wide aperture optical communications |
| CN110954506B (en) * | 2019-11-08 | 2020-10-23 | 南昌大学 | Three-parameter comprehensive measurement method for whole-layer atmospheric optical turbulence |
| CN111024245B (en) * | 2019-12-18 | 2020-12-04 | 南昌大学 | Miniaturization design method of atmospheric coherence length instrument |
| CN114355607B (en) * | 2022-01-18 | 2022-09-30 | 哈尔滨工业大学 | Non-common-path aberration self-correction method for space optical communication miniaturized terminal |
Citations (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN1940467A (en) * | 2006-08-17 | 2007-04-04 | 中国科学院光电技术研究所 | Photoelectric telescope capable of being used for high-resolution imaging and photometric measurement simultaneously |
| CN103335950A (en) * | 2013-06-24 | 2013-10-02 | 中国科学院光电技术研究所 | Device and method for measuring atmospheric turbulence non-isoplanatic wavefront error and turbulence characteristic parameters |
Family Cites Families (5)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| US4750818A (en) * | 1985-12-16 | 1988-06-14 | Cochran Gregory M | Phase conjugation method |
| CN1189774C (en) * | 1998-08-26 | 2005-02-16 | 中国科学院光电技术研究所 | Optical Wavefront Sensor |
| US7343099B2 (en) * | 2004-02-12 | 2008-03-11 | Metrologic Instruments, Inc. | Free space optical (FSO) laser communication system employing fade mitigation measures based on laser beam speckle tracking and locking principles |
| CN102169048B (en) * | 2010-12-27 | 2013-07-10 | 中国科学院光电技术研究所 | Atmospheric turbulence detection simulator for adaptive optical system |
| US8936364B2 (en) * | 2011-10-20 | 2015-01-20 | University Of Houston System | Wavefront sensorless adaptive correction of the wave aberration for an eye |
-
2015
- 2015-12-31 CN CN201511028343.XA patent/CN105466576B/en active Active
Patent Citations (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN1940467A (en) * | 2006-08-17 | 2007-04-04 | 中国科学院光电技术研究所 | Photoelectric telescope capable of being used for high-resolution imaging and photometric measurement simultaneously |
| CN103335950A (en) * | 2013-06-24 | 2013-10-02 | 中国科学院光电技术研究所 | Device and method for measuring atmospheric turbulence non-isoplanatic wavefront error and turbulence characteristic parameters |
Non-Patent Citations (2)
| Title |
|---|
| 信标湍流探测中波前非等晕问题的研究ＩＩ：实验测量;罗曦等;《中国激光》;20140630;第41卷(第6期);全文 * |
| 太阳高分辨力成像多层共轭自适应光学技术研究;张兰强;《中国博士学位论文全文数据库》;20141015(第10期);第64页 * |
Also Published As
| Publication number | Publication date |
|---|---|
| CN105466576A (en) | 2016-04-06 |
Similar Documents
| Publication | Publication Date | Title |
|---|---|---|
| CN105466576B (en) | Device and method for synchronously measuring height and angle non-isohalo wavefront errors of atmospheric turbulence | |
| CN105700128B (en) | A kind of spliced telescope common phase level control device and control method | |
| CN102252832B (en) | Wavefront quality detection device and method for large-aperture collimation system | |
| US7397540B2 (en) | Phase diversity ranging sensor | |
| CN106768876B (en) | Space solar telescope wavefront sensing methods based on asterism hot spot | |
| CN101371116B (en) | Wavefront aberration and distance measurement phase camera | |
| CN107450176B (en) | A kind of space sparse aperture telescope common phase control device and control method | |
| CN110146180B (en) | Large-view-field image sharpening device and method based on focal plane Hartmann wavefront sensor | |
| CN102122082B (en) | Phase shift error correction device of sparse optical synthetic aperture imaging system | |
| CN106644105B (en) | Wavefront sensor, detection method and system based on double helix point spread function | |
| CN108061639A (en) | Large dynamic range and high precision phase difference method wavefront measuring instrument combined with adaptive optics technology | |
| CN102636271B (en) | Phase difference method wavefront measurement imaging device based on differential optics | |
| CN111458045A (en) | Large-view-field wavefront detection method based on focal plane Hartmann wavefront sensor | |
| NL2010457C2 (en) | Hartmann wavefront measuring instrument adapted for non-uniform light illumination. | |
| CN105203213B (en) | Method for calculating composite wavefront sensing adaptive optical system recovery voltage | |
| CN111220361A (en) | Method for measuring focal length of micro-lens array | |
| CN105425378A (en) | Virtual aperture complex amplitude splicing super-resolution astronomical telescope system | |
| CN103335950A (en) | Device and method for measuring atmospheric turbulence non-isoplanatic wavefront error and turbulence characteristic parameters | |
| CN201885805U (en) | Annular common-path point diffraction-interference wave front sensing device- | |
| Huang et al. | Measurement of a large deformable aspherical mirror using SCOTS (Software Configurable Optical Test System) | |
| CN101285712B (en) | Linear phase inversion wavefront sensor based on discrete light intensity measuring device | |
| CN108955904B (en) | Multifunctional wavefront detection device considering point-surface target | |
| CN104764588B (en) | single-pulse laser dynamic focal spot position measuring device and measuring method | |
| CN108827596A (en) | One kind being applied to the novel common phase detection method of sectional type spliced telescope and device | |
| CN100562731C (en) | A kind of space reflection type optical remote sensor main mirror face deformation detecting method and system |
Legal Events
| Date | Code | Title | Description |
|---|---|---|---|
| C06 | Publication | ||
| PB01 | Publication | ||
| C10 | Entry into substantive examination | ||
| SE01 | Entry into force of request for substantive examination | ||
| GR01 | Patent grant | ||
| GR01 | Patent grant |