CN110672305A - Array type telescope multispectral common-phase error detection method for spatial modulation based on electronic shutter - Google Patents

Array type telescope multispectral common-phase error detection method for spatial modulation based on electronic shutter Download PDF

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CN110672305A
CN110672305A CN201910857304.2A CN201910857304A CN110672305A CN 110672305 A CN110672305 A CN 110672305A CN 201910857304 A CN201910857304 A CN 201910857304A CN 110672305 A CN110672305 A CN 110672305A
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telescope
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phase error
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刘柱
董理
彭起
任戈
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Institute of Optics and Electronics of CAS
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Abstract

The invention discloses an array type telescope multi-spectrum common-phase error detection method based on space modulation of an electronic shutter, which comprises the steps of firstly, adding the electronic shutter behind a beam-shrinking light path of each path of sub-telescope of an array type telescope system, and realizing pupil space modulation of the array type telescope system by controlling a shutter switch; and then, taking one path of sub-telescope as a reference aperture, sequentially acquiring a point spread function of the system, a point spread function of the reference sub-telescope and point spread functions of all other sub-telescopes, solving the common phase error distribution under the current wavelength by adopting an deconvolution method for the point spread function, respectively solving the corresponding phase distributions for different wavelengths, and finally calculating the common phase error of the whole system by utilizing a multi-spectrum synthesis algorithm. The method has simpler optical structure, and can more quickly obtain the common phase error of the array type telescope under the conditions of wider detection range and effective inhibition of 2 pi fuzzy.

Description

Array type telescope multispectral common-phase error detection method for spatial modulation based on electronic shutter
Technical Field
The invention belongs to the field of imaging of array telescopes, and particularly relates to an array telescope multispectral common-phase error detection method for performing spatial modulation based on an electronic shutter.
Background
The light collecting capacity and the resolution ratio are two most important performance indexes of the telescope, and the stable improvement of the two parameters depends on the continuous increase of the aperture of the telescope. The single aperture size of the telescope is limited in ten meters range due to manufacturing process and material cost, the optical synthetic aperture imaging technology is produced, the multi-path separated sub-telescope systems are spliced or combined, so that the resolution of the system reaches the resolution of an equivalent large aperture telescope, and meanwhile, the system has the advantages of small aperture of the sub-telescope, easy manufacture of a single mirror surface, low cost, small volume, light weight, easy transportation, flexible assembly and the like, the difficult problem of large single aperture telescopes can be solved, and the hope is brought to the acquisition of telescope systems with higher resolution for people.
The common-phase error detection technology has been widely studied by scientific research institutions in related fields because the optical synthetic aperture imaging system can realize common-phase and improve resolution. The research on the technology is carried out later in China, and the institutions for researching the technology mainly comprise Harbin industry university, Changchun optical precision machinery and physical research institute of Chinese academy of sciences, photoelectric technology research institute of Chinese academy of sciences and the like. At present, the technology is gradually transferred to practical application from theoretical research, in the practical application process, in order to ensure the imaging quality of the whole telescope system, the root mean square value of the common phase error among all the sub-mirrors needs to be controlled within 0.1 lambda, but most of the existing common phase error detection methods have the defects of complex algorithm, multiple iteration times, small detection interval, 2 pi fuzzy influence and the like, so the research on the common phase detection technology has great practical significance at present.
Disclosure of Invention
The invention aims to provide an array type telescope multispectral common-phase error detection method for carrying out spatial modulation based on an electronic shutter, which can more quickly obtain the common-phase error of an array type telescope under the condition of wider detection range and effectively inhibit 2 pi fuzzy.
The technical solution adopted by the invention is as follows: an array type telescope multispectral common-phase error detection method based on electronic shutter for space modulation is used for common-phase detection of an array type telescope system and comprises the following specific steps:
step one, building a light path:
firstly, building an experimental light path as shown in fig. 2 on an experimental platform; the experimental light path refers to an array type telescope system light path;
firstly, a multi-wavelength light source is arranged on the leftmost side, light from the light source is converted into parallel light through a beam expanding system, most of the emitted parallel light is divided into N paths of sub-light paths through a plurality of 45-degree plane reflectors which are parallel to each other, the sub-light path of each path is contracted through a Cassegrain telescope, the contracted light path is subjected to spatial modulation through an electronic shutter, then the propagation direction of the light path is changed through the plane reflectors, and the light passes through another Cassegrain telescope system to be imaged with light of a reference light path; the rest parallel light from the beam expanding system is taken as a reference light path, directly passes through another Cassegrain telescope for beam contraction, then is subjected to light path adjustment by a plane reflector, and finally is imaged with other N paths of light through the Cassegrain telescope system. And finally, receiving the formed image by an area array detector.
Step two, system aperture modulation:
firstly, selecting the wavelength as lambda1Assuming that the system has N +1 sub-telescopes, each sub-telescope is modulated by the added electronic shutter;
then selecting a path of sub-telescope at the edge as reference, and measuring the point spread function of the sub-telescope as PSF (point spread function) by using a detection device1(P); the point spread function of the remaining N sub-paths is PSFN(P), and point spread function PSF of the systemN+1(P)；
Step three optical transfer function solution
Obtaining the corresponding optical transfer function OTF from the three point spread functions1(P)，OTFN(P),OTFN+1(P) there is the following relationship between them:
Figure RE-GDA0002268933710000021
wherein B is1Pupil as reference pupilFunction, BNRepresenting the pupil function of the sub-telescope to be measured, PnIs the central coordinate of the nth sub-telescope, Delta (P-P)n) For the wavefront distribution of the nth sub-telescope, the symbol denotes the convolution operation, OTF1(P) and OTFN(P) represents the optical transfer function of the reference pupil and all pupils of the N-way, respectively.
Step four, calculation of phase distribution:
by performing a series of fourier transform product operations on the above equation, one can obtain:
Figure RE-GDA0002268933710000031
after the phase distribution of the formula is obtained by deconvolution, the phase of the first part on the right side is only needed to obtain the phase distribution of the system at lambda1Phase distribution at wavelength
And fifthly, calculating the common phase error:
sequentially converting the wavelength of the point light source in the step two into lambda2，λ3Repeating the second step, the third step and the fourth step to obtain phi respectively2n，φ3nIf the phase sharing error Δ of the nth sub-mirror is:
Δ＝(n1+φ1n)λ1＝(n2+φ2n)λ2＝(n3+φ3n)λ3
because the above equation is an under-constrained equation, the synthetic wavelength λ is defined:
λ＝(1/λ1-2/λ2+1/λ3)-1
by using the synthesis wavelength and the under-constrained equation and combining the multi-spectrum synthesis algorithm, the co-phase error delta can be solved.
The principle of the invention is as follows: the method comprises the steps of utilizing an electronic shutter to perform spatial modulation on each path of sub-telescope, utilizing an area array detector on a system focal plane to obtain point spread functions of the sub-telescopes and the system, then utilizing deconvolution to obtain phase distribution under the wavelength condition, but because the single wavelength has 2 pi fuzzy influence, under the condition, the wavelength of a point light source is replaced for many times, and according to the previous steps, the phase distribution under the respective wavelength condition is respectively obtained, all phase distribution equations are combined to obtain an under-constrained equation, then assuming an equation of a synthesized wavelength, and combining the equations to obtain the common-phase error distribution of the system by utilizing a multi-spectrum synthesis algorithm.
Compared with the prior art, the invention has the following advantages:
(1) the electronic shutter is used for carrying out spatial modulation on each sub-telescope of the system, so that the system is simpler in structure;
(2) in the solving process of the single-wavelength phase distribution, a deconvolution method is used for replacing and additionally introducing a small-size reference pupil, so that the system structure can be effectively simplified, and a series of problems caused by the small-size reference pupil are completely avoided;
(3) the application of the multi-spectrum synthesis algorithm effectively improves the real-time performance of detection;
(4) the application of a plurality of light sources with different wavelengths effectively removes the influence of 2 pi blurring and improves the detection range of the system common phase error.
Drawings
FIG. 1 is a flow chart of a multispectral co-phasing error detection method based on pupil spatial modulation;
fig. 2 is an optical path diagram of the three sub-telescope system.
Detailed Description
The embodiments of the present invention will be further described with reference to the accompanying drawings and specific implementation steps.
As shown in the flowchart of fig. 1, the method for detecting multispectral co-phasing error based on pupil spatial modulation comprises the following steps:
step one, building a light path:
firstly, building an experimental light path as shown in fig. 2 on an experimental platform; firstly, a multi-wavelength light source is arranged on the leftmost side, light from the light source is converted into parallel light through a beam expanding system, most of the emitted parallel light is divided into N paths of sub-light paths through a plurality of 45-degree plane reflectors which are parallel to each other, the sub-light path of each path is contracted through a Cassegrain telescope, the contracted light path is subjected to spatial modulation through an electronic shutter, then the propagation direction of the light path is changed through the plane reflectors, and the light passes through another Cassegrain telescope system to be imaged with light of a reference light path; the rest parallel light from the beam expanding system is taken as a reference light path, directly passes through another Cassegrain telescope for beam contraction, then is subjected to light path adjustment by a plane reflector, and finally is imaged with other N paths of light through the Cassegrain telescope system. And finally, receiving the formed image by an area array detector.
Pupil spatial modulation:
firstly, selecting the wavelength as lambda1Assuming that the system has N +1 sub-telescopes, each sub-telescope is modulated by the added electronic shutter;
then selecting a path of sub-telescope at the edge as reference, and measuring the point spread function of the sub-telescope as PSF (point spread function) by using a detection device1(P); the point spread function of the remaining N sub-paths is PSFN(P), and point spread function PSF of the systemN+1(P)；
Step three, solving an optical transfer function:
obtaining the corresponding optical transfer function OTF from the three point spread functions1(P)，OTFN(P),OTFN+1(P) there is the following relationship between them:
wherein B is1As a pupil function of a reference pupil, B2Representing the pupil function of the sub-telescope to be measured, PnIs the central coordinate of the nth sub-telescope, Delta (P-P)n) For the wavefront distribution of the nth sub-telescope, the symbol denotes the convolution operation, OTF1(P) and OTF2(P) represents the optical transfer function of the reference pupil and all pupils of the 2-way, respectively.
Step four, calculation of phase distribution:
by performing a series of fourier transform product operations on the above equation, one can obtain:
Figure RE-GDA0002268933710000051
after the phase distribution of the formula is obtained by deconvolution, the phase of the first part on the right side is only needed to obtain the phase distribution of the system at lambda1Phase distribution phi at wavelength1A phase profile can be obtained.
And fifthly, calculating the common phase error:
sequentially converting the wavelength of the point light source in the step two into lambda2，λ3Repeating the second step, the third step and the fourth step to obtain phi respectively2，φ3If the phase sharing error Δ of the nth sub-mirror is:
Δ＝(n1+φ1)λ1＝(n2+φ2)λ2＝(n3+φ3)λ3
because the above equation is an under-constrained equation, the synthetic wavelength λ is defined:
λ＝(1/λ1-2/λ2+1/λ3)-1
by using the synthesis wavelength and the under-constrained equation and combining the multi-spectrum synthesis algorithm, the co-phase error delta can be solved.

Claims (6)

1. An array type telescope multispectral common-phase error detection method based on electronic shutter for space modulation is used for common-phase error detection among sub-mirrors of an array type telescope system and is characterized by comprising the following steps:
step one, building a light path:
firstly, building an experimental light path on an experimental platform; the experimental light path refers to an array type telescope system light path;
step two, system aperture modulation:
firstly, selecting the wavelength as lambda1Monochromatic light of, say, systemThe total number of the N +1 sub-telescopes is N, and each sub-telescope is modulated through an added electronic shutter;
then selecting a path of sub-telescope at the edge as reference, and measuring the point spread function of the sub-telescope as PSF (point spread function) by using a detection device1(P); the point spread function of the remaining N sub-paths is PSFN(P), and point spread function PSF of the systemN+1(P)；
Step three, solving an optical transfer function:
obtaining the corresponding optical transfer function OTF from the three point spread functions1(P)，OTFN(P),OTFN+1(P) there is the following relationship between them:
Figure FDA0002198687930000011
wherein B is1As a function of the pupil of the reference aperture, BNRepresenting the pupil function of the sub-telescope to be measured, PnIs the central coordinate of the nth sub-telescope, Delta (P-P)n) For the wavefront distribution of the nth sub-telescope, the symbol denotes the convolution operation, OTF1(P) and OTFN(P) representing the optical transfer functions of the reference aperture and all the apertures of the N paths, respectively;
step four, calculation of phase distribution:
by performing a series of fourier transform product operations on the above equation, one can obtain:
Figure FDA0002198687930000012
after the phase distribution of the formula is obtained by deconvolution, the phase of the first part on the right side is only needed to obtain the phase distribution of the system at lambda1Phase distribution at wavelength
Figure FDA0002198687930000013
And fifthly, calculating the common phase error:
sequentially converting the wavelength of the point light source in the step two into lambda2，λ3Repeating the second step, the third step and the fourth step to obtain phi respectively2n，φ3nIf the phase sharing error Δ of the nth sub-mirror is:
Δ＝(n1+φ1n)λ1＝(n2+φ2n)λ2＝(n3+φ3n)λ3
because the above equation is an under-constrained equation, the synthetic wavelength λ is defined:
λ＝(1/λ1-2/λ2+1/λ3)-1
by using the synthesis wavelength and the under-constrained equation and combining the multi-spectrum synthesis algorithm, the co-phase error delta can be solved.
2. The method as claimed in claim 1, wherein the λ in step two is λ1And lambda in step five2，λ3Refers to any random wavelength.
3. The method as claimed in claim 1, wherein the point light source in step two can be replaced by a broadband light source in combination with a narrow band filter.
4. The method as claimed in claim 1, wherein the electronic shutter in step two is a diaphragm or other device capable of rapidly blocking the optical path.
5. The method as claimed in claim 1, wherein the detector in step two is a CCD camera, a CMOS camera or other area-array detector.
6. The method as claimed in claim 1, wherein the step five is performed by sequentially selecting λ2，λ3In fact, two wavelengths, but not limited to two wavelengths, can be selected for processing, i.e., more different wavelengths can be selected to replace the two wavelengths in this step.
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Publication number Priority date Publication date Assignee Title
CN113029526A (en) * 2021-03-10 2021-06-25 中国科学院长春光学精密机械与物理研究所 Synthetic aperture co-phasing error estimation method and device

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Publication number Priority date Publication date Assignee Title
CN107656363A (en) * 2017-10-31 2018-02-02 中国科学院光电技术研究所 A kind of optical synthesis aperture imaging telescope array common phase error detection method based on multi-wavelength phase-modulation

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Publication number Priority date Publication date Assignee Title
CN107656363A (en) * 2017-10-31 2018-02-02 中国科学院光电技术研究所 A kind of optical synthesis aperture imaging telescope array common phase error detection method based on multi-wavelength phase-modulation

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董理: "合成孔径望远镜共相误差多谱探测技术研究", 《中国博士学位论文全文数据库 工程科技Ⅱ辑》 *

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Publication number Priority date Publication date Assignee Title
CN113029526A (en) * 2021-03-10 2021-06-25 中国科学院长春光学精密机械与物理研究所 Synthetic aperture co-phasing error estimation method and device
CN113029526B (en) * 2021-03-10 2022-11-11 中国科学院长春光学精密机械与物理研究所 Synthetic aperture co-phasing error estimation method and device

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