CN107966280B - Photoelectric detection system applied to spliced telescope and rapid common-phase adjustment method thereof - Google Patents
Photoelectric detection system applied to spliced telescope and rapid common-phase adjustment method thereof Download PDFInfo
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Abstract
A photoelectric detection system applied to a spliced telescope comprises a collimating lens, a small spliced mirror, a 4f system, a spectroscope, an optical filter, a spliced mirror MASK, a shack Hartmann wavefront detector, an imaging system and a control system. By utilizing the photoelectric detection system, far-field light spot information between adjacent splicing sub-mirrors is obtained through a shack Hartmann wavefront detector, and a translation (piston) error between the adjacent sub-mirrors is rapidly calculated by utilizing a dual-wavelength detection method; the small splicing mirror piston error is quickly adjusted through a control system, so that the purpose of the piston error of quick phase-sharing adjustment is achieved; the system achieves the purpose of quickly adjusting the piston error of the splicing mirror system by adjusting the small splicing mirror instead of adjusting the splicing mirror.
Description
Technical Field
The invention relates to a photoelectric detection system, in particular to a photoelectric detection system for a splicing mirror and a rapid common-phase adjusting method.
Background
The telescope resolution is related to factors such as atmospheric turbulence, telescope caliber and observation light wavelength. If the influence of factors such as atmospheric turbulence and the like is neglected and the size of the observation light wavelength is fixed, the aperture of the telescope needs to be increased continuously in order to detect a more remote and darker celestial body. At present, three design schemes are provided for manufacturing a large-caliber telescope: a thin primary mirror, a honeycomb mirror, and a splice mirror. However, the optical telescope with single caliber cannot be infinitely increased due to the manufacturing technology, the processing cost, the risk factors and the like. At present, the aperture limit of a primary mirror of a single-block optical telescope is 8.4 m. If an optical telescope with a larger caliber is manufactured, a splicing mirror technology is adopted. However, the use of the tiled mirror technique also presents many new challenges, the most important of which is the problem of detecting the translation error (piston) between the sub-mirrors. Only when the splicing mirrors are in phase, the imaging quality equivalent to that of a single-mirror primary mirror system with the same aperture can be achieved. In order to obtain good image quality of the splicing telescope, the pixel error of the system needs to be controlled at 100nm.
At present, 10-meter-scale spliced telescopes (American Hawaii keck telescope and Spanish GTC telescope) which are in operation, 30-meter spliced telescopes (American TMT telescope) and 39-meter spliced telescopes (European southern astronomical stage E-ELT telescope) which are to be built are adjusted to achieve the aim of common-phase adjustment by adjusting the piston error of the primary mirror of the spliced telescope. However, the aperture of the single spliced sub-mirror is more than 1 meter, and the momentum and the resonance frequency are low, so that the speed of adjusting the common phase is low. The spliced telescope can not realize the purpose of fast phase sharing, thereby being incapable of realizing the purpose of fast observing objects.
Prior art references: (1) an invention patent with an authorization publication number of CN 101694414B; (2) the invention patent application with publication number CN 101276056 a; (3) li bin, study of a splicing mirror co-phase detection technology [ D ]. beijing, institute of graduate college of chinese academy of sciences 2017.
Disclosure of Invention
Aiming at the problem of low common-phase adjustment speed of a splicing mirror system, the invention aims to provide a photoelectric detection system applied to rapid common-phase adjustment of a splicing mirror. The photoelectric detection system achieves the purpose of quickly detecting the piston error of the splicing lens by placing a small splicing lens on the conjugate surface of the primary lens of the splicing telescope and achieving the purpose of quickly adjusting the piston error in the telescope system by quickly adjusting the piston error of the small splicing lens.
The technical scheme for solving the problems is as follows:
a photoelectric detection system applied to a spliced telescope comprises a collimating lens, a small splicing mirror, a 4f system, a first beam splitter prism, a splicing mirror MASK, a second beam splitter prism, a first narrow band optical filter, a first shack Hartmann wavefront detector, a second narrow band optical filter, a second shack Hartmann wavefront detector, a third beam splitter prism, a third shack Hartmann wavefront detector, an imaging system, a piezoelectric ceramic actuator and a control system;
the small splicing lens is arranged on a conjugate surface of the splicing telescope, and a collimating lens is arranged between the splicing telescope and the small splicing lens, wherein the number of sub-lenses of the small splicing lens is the same as that of the splicing telescope; the collimating lens is used for converting light received by the splicing telescope into parallel light and then transmitting the parallel light to the small splicing lens, and the small splicing lens is used for reflecting the parallel light coming out of the collimating lens to the 4f system;
a 4f system is arranged between the small splicing mirror and the first light splitting prism, and a second light splitting prism and a third light splitting prism are respectively arranged in two light splitting directions of the first light splitting prism; a splicing lens MASK is arranged between the first beam splitter prism and the second beam splitter prism;
the first shack Hartmann wavefront detector and the second shack Hartmann wavefront detector are respectively arranged in the two light splitting directions of the second light splitting prism; a first optical filter is arranged between the first shack Hartmann wavefront detector and the second shack Hartmann wavefront detector;
a third shack Hartmann wavefront detector and an imaging system are respectively arranged in the two light splitting directions of the third light splitting prism;
the piezoelectric ceramic actuator is connected with the small splicing mirror and is used for driving the small splicing mirror to move;
the control system is respectively connected with the first shack Hartmann wavefront detector, the second shack Hartmann wavefront detector, the third shack Hartmann wavefront detector, the imaging system and the piezoelectric ceramic actuator.
Each sub-mirror of the small splicing mirror is provided with three supporting points, piezoelectric ceramic actuators are arranged on the three supporting points and distributed on the same circle, and a capacitance sensor is arranged at the central symmetrical position of each supporting point; the control system controls the deformation of the piezoelectric ceramic actuator in a closed loop mode through the value of the capacitance sensor, and then controls the movement of the small splicing mirror.
The method for realizing the rapid phase sharing regulation comprises the following steps:
the splicing telescope receives light waves, because tilt and piston errors exist among splicing sub-mirrors, the received light waves are discontinuous, the received light waves are collimated into parallel light through a collimating lens and then reflected through a small splicing mirror, the small splicing mirror is placed on a conjugate surface of a main mirror of the splicing telescope and sequentially passes through a 4f system and a first light splitting prism, a part of light is shielded by MASK and then split by a second light splitting prism, and then the light is respectively filtered by a first narrow band light filter and a second narrow band light filter and respectively enters a first shack Hartmann wavefront detector and a second shack Hartmann wavefront detector; the rest light enters a third beam splitter prism, one part of the light enters a third CharkerHartmann wavefront detector, and the other part of the light enters an imaging system;
light beams entering the first shack Hartmann wavefront detector and the second shack Hartmann wavefront detector respectively present far-field light spots between two spliced sub-mirrors under a certain narrow-band light on the CCD, a double-wave detection method is utilized to calculate the piston error between the adjacent sub-mirrors, and finally a control system controls a piezoelectric ceramic actuator behind the small spliced mirror to achieve the purpose of quickly adjusting the piston error of the spliced mirror system;
and the other part of the light beam enters a third Charcot Hartmann wavefront detector, a series of diffraction light spots are formed on the CCD, the diffraction light spots are deviated from the azimuth and the distance of the standard position through a control system, the inclination error of the splicing sub-mirror is calculated, and the control system controls a piezoelectric ceramic actuator behind the small splicing mirror to adjust the inclination error of the splicing mirror.
The imaging system comprises a self-adaptive system, an observation system and the like, wherein the self-adaptive system is used for correcting the influence of atmospheric turbulence on the quality of light waves, and the observation system is used for observing celestial body information.
Compared with the prior art, the invention has the following advantages:
1) the method for detecting the piston error by adopting the dual-wavelength method achieves the purpose of quickly detecting the piston error.
2) And small splicing mirrors which are in one-to-one correspondence with the splicing mirrors are arranged on the conjugate surface of the splicing primary mirror in the splicing mirror telescope optical path system, and the purpose of adjusting the piston error in the splicing telescope system is achieved by adjusting the piston error of the small splicing mirrors. The aperture of the small splicing sub-mirror is in the order of tens of millimeters, so that the small splicing sub-mirror has small inertia and large resonance frequency, and the purpose of rapid phase-sharing adjustment can be achieved.
Drawings
Fig. 1 is a schematic diagram of the device composition and principle of the photoelectric detection system of the present invention.
Fig. 2 is a schematic diagram of a microlens array in a third shack hartmann wavefront sensor.
FIG. 3 is a diagram showing MASK distribution.
FIG. 4 is a schematic diagram of the distribution of piezoelectric ceramic actuators of a small splice mirror.
Fig. 5 is a schematic diagram of the control system.
In the figure, a splicing telescope (1), a collimating lens (2), a small splicing mirror (3), a 4f system (4), a first beam splitter prism (5), a splicing mirror MASK (6), a second beam splitter prism (7), a first optical filter (8), a first shack Hartmann wavefront detector (9), a second optical filter (10), a second shack Hartmann wavefront detector (11), a second beam splitter prism (12), a third shack Hartmann wavefront detector (13), an imaging system (14) and a control system (15).
Detailed Description
As shown in fig. 1, a photoelectric detection system applied to a splicing telescope includes: the device comprises a collimating lens 2, a small splicing mirror 3, a 4f system 4, a first beam splitter prism 5, a splicing mirror MASK 6, a second beam splitter prism 7, a first optical filter 8, a first shack Hartmann wavefront detector 9, a second optical filter 10, a second shack Hartmann wavefront detector 11, a second beam splitter prism 12, a third shack Hartmann wavefront detector 13, an imaging system 14 and a control system 15. Wherein, the small splicing lens 3 is arranged on the conjugate surface of the primary mirror of the splicing telescope. In the present embodiment, the splicing telescope 1 includes four sub-mirrors, and therefore the small splicing mirror 3 also includes four sub-mirrors.
As shown in fig. 2, the hartmann micro lens array is divided into four parts, each region corresponds to one splicing sub-mirror, and light forms diffraction light spots on the high frame frequency CCD target surface after entering the micro lens array; calculating the central position (x, y) of each area spot by adopting a centroid algorithm, comparing the central position (x, y) with a calibration position (0, 0), and respectively calculating the wavefront phase tilt amount and the tilt direction;
wherein the content of the first and second substances,
is the amount of wavefront phase tilt, unitIs nm, where α is the telescope angular magnification, f is the microlens focal length, and D is the primary mirror size; θ is the wavefront phase tilt phase.
The data processor of the control system 15 controls the tilt angle of the small splicing mirror according to the data collected by the high frame frequency CCD, and compensates the tilt error of the splicing mirror in real time.
As shown in fig. 3, after a light beam enters a mask 6, most of the light beam is blocked, and then the light beam irradiates a micro-array lens, wherein the micro-array sub-lens corresponds to a circular hole in the mask, 5 circular hole diffraction patterns are obtained by imaging on a CCD, a biston error of two adjacent sub-lenses can be calculated by using a dual-wavelength detection method according to the circular hole pattern information, and a certain sub-lens is taken as a reference, so that a mosaic lens biston error is obtained.
As shown in fig. 4, the small splice mirror 3 has 3 supporting points, the supporting points are controlled by piezoelectric ceramic actuators and distributed on the same circle, and a capacitance sensor is placed at the central symmetrical position of each supporting point; the control system controls the deformation of the piezoelectric ceramic actuator in a closed loop mode through the value of the capacitance sensor, and then controls the movement of the small splicing mirror.
As shown in fig. 5, with reference to a certain sub-mirror, after the light wave passes through shack hartmann 9, shack hartmann 11 and shack hartmann 13, the tilt amount and the translation amount of other sub-mirrors can be calculated and converted into the value of each sub-mirror capacitance sensor, and the deformation amount of the piezoelectric ceramic actuator is controlled in a closed loop manner by the value of the capacitance sensor.
The imaging system 14 includes an adaptive system for correcting the influence of the atmospheric turbulence on the quality of the optical waves, an observation system for observing celestial body information, and the like.
The number of the spliced sub-mirrors in the device is 4, and the change of the number of the spliced sub-mirrors and the improvement of a telescope system, which change the essence and the core function of the invention, belong to the scope of the invention.
The change of the aperture size of the small splicing sub-mirror, the type of the piezoelectric ceramic actuator and the type of the sensor, and the change of the essence and the core function of the invention belong to the scope of the invention.
In the invention, only the shack Hartmann method is used for detecting the tilt error of the splicing lens, and other confocal detection methods are used for calculating the tilt error of the splicing lens, which also belongs to the scope of the invention.
Claims (3)
1. A quick common-phase adjusting method applied to a splicing telescope is characterized by comprising the following steps: arranging a small splicing mirror on a conjugate surface of the splicing telescope, and detecting light received by the splicing telescope after the light is reflected by the small splicing mirror to obtain far-field light spot information and diffraction light spot information between two adjacent sub-mirrors; then respectively calculating a piston error and a tilt error between two adjacent sub-mirrors according to the far-field light spot information and the diffraction light spot information; finally, the small splicing mirror is adjusted according to the piston error and the inclination error, and the purpose of quickly and commonly adjusting the splicing telescope and the small splicing mirror system is achieved; the method specifically comprises the following steps:
(1) the light received by the splicing telescope is changed into parallel light by utilizing a collimating lens and is emitted;
(2) a small splicing mirror is arranged behind the collimating lens and is positioned on a conjugate surface of the splicing telescope, the number of sub-mirrors of the small splicing mirror is the same as that of the splicing telescope, and the parallel light from the collimating lens is reflected to a 4f system by the small splicing mirror;
(3) the light emitted from the 4f system is divided into two parts by using a first light splitting prism, and one part of the light respectively enters a first shack Hartmann wavefront detector and a second shack Hartmann wavefront detector after sequentially passing through a splicing lens MASK and a second light splitting prism; the other part of light enters a third Charcot Hartmann wavefront detector and an imaging system respectively after passing through a light splitting prism;
(4) light beams entering the first shack Hartmann wavefront detector and the second shack Hartmann wavefront detector respectively present far-field light spots between two adjacent spliced sub-mirrors under a certain narrow-band light on the CCD, a pixel error between the two adjacent sub-mirrors is calculated by using a double-wave detection principle, and a piezoelectric ceramic actuator is controlled by a control system to adjust the small spliced mirror according to the pixel error; a light beam entering the third shack Hartmann wavefront detector forms a series of diffraction light spots on the CCD, the diffraction light spots are deviated from the azimuth and the distance of a standard position through the control system, the inclination error of two adjacent sub-mirrors is calculated, and the control system is utilized to control the piezoelectric ceramic actuator to adjust the small splicing mirror according to the inclination error;
calculating the central position (x, y) of each area spot by adopting a centroid algorithm, comparing the central position (x, y) with a calibration position (0, 0), and respectively calculating the wavefront phase inclination amount and the inclination direction;
wherein, DeltaφIs the wavefront phase tilt in nm, where alpha is the telescope angular magnification,fis the focal length of the micro-lens,Dis the primary mirror size;θtilting the phase for the wavefront phase;
and a data processor of the control system controls the inclination angle of the small splicing mirror according to the data collected by the CCD, and compensates the inclination error of the splicing mirror in real time.
2. A photoelectric detection system applied to a spliced telescope comprises a collimating lens, a small splicing mirror, a 4f system, a first beam splitter prism, a splicing mirror MASK, a second beam splitter prism, a first optical filter, a first shack Hartmann wavefront detector, a second optical filter, a second shack Hartmann wavefront detector, a third beam splitter prism, a third shack Hartmann wavefront detector, an imaging system, a piezoelectric ceramic actuator and a control system;
the small splicing lens is arranged on a conjugate surface of the splicing telescope, and a collimating lens is arranged between the splicing telescope and the small splicing lens, wherein the number of sub-lenses of the small splicing lens is the same as that of the splicing telescope; the collimating lens is used for converting light received by the splicing telescope into parallel light and then transmitting the parallel light to the small splicing lens, and the small splicing lens is used for reflecting the parallel light coming out of the collimating lens to the 4f system;
a 4f system is arranged between the small splicing mirror and the first light splitting prism, and a second light splitting prism and a third light splitting prism are respectively arranged in two light splitting directions of the first light splitting prism; a splicing lens MASK is arranged between the first beam splitter prism and the second beam splitter prism;
the first shack Hartmann wavefront detector and the second shack Hartmann wavefront detector are respectively arranged in the two light splitting directions of the second light splitting prism; a first optical filter is arranged between the first shack Hartmann wavefront detector and the second shack Hartmann wavefront detector;
a third shack Hartmann wavefront detector and an imaging system are respectively arranged in the two light splitting directions of the third light splitting prism;
the piezoelectric ceramic actuator is connected with the small splicing mirror and is used for driving the small splicing mirror to move;
the control system is respectively connected with the first shack Hartmann wavefront detector, the second shack Hartmann wavefront detector, the third shack Hartmann wavefront detector, the imaging system and the piezoelectric ceramic actuator.
3. The photoelectric detection system applied to the splicing telescope of claim 2, wherein: each sub-mirror of the small splicing mirror is provided with three supporting points, piezoelectric ceramic actuators are arranged on the three supporting points and are distributed on the same circle, and a capacitance sensor is arranged at the central symmetrical position of each supporting point; the control system controls the deformation of the piezoelectric ceramic actuator through the capacitance sensor, and then controls the movement of the small splicing mirror.
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