CN113029365A - Large-view-field high-order composite wavefront sensor for solar adaptive optics - Google Patents
Large-view-field high-order composite wavefront sensor for solar adaptive optics Download PDFInfo
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Abstract
The invention provides a large-field-of-view high-order composite wavefront sensor for solar adaptive optics, which comprises an image plane divider (1), a relay light path (2), a micro lens array (3) and a corresponding detection camera (4). The image plane divider (1) divides an image plane and then guides the divided image plane into different detection channels, each detection channel comprises a relay light path (2), a micro lens array (3) and a detection camera (4), and wavefront detection is carried out on a specific view field. The central view field detection adopts a small view field high-order wavefront sensor, and the off-axis view field adopts a large view field low-order wavefront sensor. The invention cuts the image surface of the large view field of the telescope based on the image surface divider, and then uses a plurality of discrete shack-Hartmann wavefront sensors to detect the wavefronts of different view fields, thereby realizing the wavefront detection of the oversized view field. The invention simultaneously meets different requirements of the traditional high-order adaptive optical system and the large-field-of-view ground surface layer adaptive optical system on the wavefront detector.
Description
Technical Field
The invention belongs to the field of adaptive optics, mainly relates to a wavefront detection technology in a solar adaptive optical system, in particular to a composite wavefront detection technology considering both a large traditional high-order solar adaptive optical system and a large-view-field low-order surface layer adaptive optical system, and particularly relates to a large-view-field high-order composite wavefront sensor for solar adaptive optics.
Background
A solar Adaptive Optics (AO) system is one of necessary means for successfully realizing high-resolution imaging observation of solar atmosphere by a foundation large-caliber solar telescope at home and abroad. The ground-based solar telescope is influenced by atmospheric turbulence, and the spatial resolution cannot exceed the resolution capability of a telescope with a 20cm caliber. Therefore, an adaptive optical system is required to be equipped for the large-aperture solar telescope, and the imaging capability of the large-aperture solar telescope is fully exerted by detecting and compensating the atmospheric turbulence in real time so as to enable the large-aperture solar telescope to reach or approach the observation performance of the diffraction limit. The self-adaptive optical system is limited by the non-isosickness of the atmosphere, the correction field of view is very limited, and the correction field of view is only in the order of magnitude of angular seconds in a visible light wave band, so that the high-resolution imaging observation requirement of the sun on the physical diagonal component level sun active area can not be met. Various large-field-of-view adaptive optics technologies, especially surface layer adaptive optics (GLAO), are proposed, and the contradiction is well solved.
Surface adaptive optics follow the concept of layered detection and correction to correct for surface turbulence that occupies the major component of atmospheric turbulence. The GLAO correction can improve the imaging quality of the system in a large view field range although the GLAO correction cannot reach the diffraction limit, and has important significance for large view field monitoring of a solar active area. Because the light rays of different sight lines pass through the same area on the surface of the ground when passing through the atmosphere and are separated from each other on the high layer, the accumulated wavefront errors in a plurality of sight line directions can be detected firstly, and then the turbulence on the surface of the ground can be extracted based on an average algorithm. The prevailing view is that GLAO technology will play an important role in solar observation. If the traditional adaptive optics and the GLAO can be combined, the large-view-field monitoring and the small-view-field diffraction limit imaging of the solar active area are realized. Has important application value. Since both the GLAO and the conventional AO employ a single-block wavefront corrector, both can be shared, with the difference being the wavefront sensor.
For a solar adaptive optics system, wavefront detection needs to adopt a correlated shack-hartmann wavefront sensor based on a cross-correlation algorithm. Different from point source target detection in a night astronomical adaptive optical system, each sub-aperture of a relevant shack-Hartmann wavefront sensor needs to correspond to a certain detection field of view, so that the wavefront aberration of different sub-apertures can be extracted by carrying out relevant operation on AN image with certain expansion degree, and for a solar large-field adaptive optical technology, large-field multi-sight wavefront detection (D.Soltau, T.Berkefeld, el al Astron.Nachr./AN 3233/4, 236-240, 2002) can be realized by increasing the detection field of view of the wavefront sensor. However, such wavefront sensors face a contradiction between the number of sub-apertures and the field of view of detection. In order to keep the accuracy of the correlation algorithm, the wavefront sensor needs to maintain a certain pixel resolution, and on the premise, in the wavefront sensor with a specific detection view field, the camera target surface corresponding to each sub-aperture is certain, and the larger the number of the sub-apertures is, the larger the detection view field is, the larger the required detection camera target surface is. But is limited by the detector technology itself and takes into account the temporal frame rate requirements of adaptive optics for detecting the kilohertz. A trade-off must be made between the two. Generally speaking, a large-field wavefront sensor has few corresponding sub-apertures and cannot perform high-order wavefront detection. In addition, because the number of the sub-apertures of the large-field shack-Hartmann wavefront sensor is not matched with the number of the correction drivers of the deformable mirror, in order to measure the transfer function of the control system, an additional wavefront sensor matched with the number of the drivers of the deformable mirror is required to be additionally assisted. Aiming at the technical level of the current COMS camera, the large-field wavefront sensor can only meet the detection requirement of a meter-class aperture telescope on an angular-division-level field. For the wavefront detection of a larger-aperture telescope or a larger-view-field (5-10 angular division magnitude) GLAO system, the multi-sight wavefront detection can be realized only by splitting a focal plane and providing a plurality of independent wavefront sensors. For example, in a large-field MCAO system on a four-meter solar telescope DKIST in the united states, wavefront detection in 9 sight directions is realized by splitting a focal plane (d.schmidt, j.marino, et al, SPIE vol.107032018). This detection mode detects a field of view that increases in synchronism with system cost and hardware complexity. For the GLAO detection mode, the more fields of view detected, the more accurate the average algorithm gets for surface layer turbulence. The wavefront sensor of the DKIST telescope is not an ideal choice.
The invention provides a composite type high-order wavefront sensor with a large view field aiming at the problems of the two wavefront sensors. The wavefront sensor is in a large-view-field low-order/small-view-field high-order wavefront sensor combination mode, so that the detection requirement of a GLAO system on more realization directions in a larger view field range is met.
Disclosure of Invention
The technical problem to be solved by the invention is as follows: aiming at the requirements of solar physics research on large-view-field high-resolution monitoring and small-view-field diffraction limit imaging of the solar atmosphere, the invention provides a large-view-field high-order composite wavefront sensor for solar adaptive optics, aiming at the technical problem that a wavefront detection view field and detection precision (detection order) are contradictory in the solar adaptive optics technology. The invention cuts the image surface of the large view field of the telescope based on the image surface divider, and then uses a plurality of discrete shack-Hartmann wavefront sensors to detect the wavefronts of different view fields, thereby realizing the wavefront detection of the oversized view field. By the combination of the large-view-field low-order/small-view-field high-order shack-Hartmann wavefront sensor, different requirements of a traditional high-order adaptive optical system and a large-view-field surface layer adaptive optical system on a wavefront detector are met. The method has clear application value in the application fields of solar active area monitoring and the like which have the requirements of large-view-field high-resolution monitoring and small-view-field diffraction limit imaging.
The technical scheme adopted by the invention for solving the technical problems is as follows: a large-view-field high-order composite wavefront sensor for solar adaptive optics comprises an image plane divider, a relay light path, a micro lens array and corresponding detection cameras; the image plane divider divides an image plane and then guides the image plane into different detection channels, each detection channel comprises a relay light path, a micro lens array and a detector, and wavefront detection is carried out on a specific view field. After the image plane splitter divides the focal plane of the telescope, the focal plane of the telescope is respectively guided to enter different detection channels; wherein, the on-axis detection channel corresponds to a dozen angular seconds detection field of view, and the off-axis detection channel corresponds to an angularly graded detection field of view. The method comprises the steps that a large-field-of-view wavefront sensor is arranged on an off-axis detection channel, detection information in different sight directions can be obtained by selecting different sub-regions of a sub-aperture image, and more accumulated wavefront aberrations of detection fields can be obtained under the condition of the same detection channel; the on-axis channel only allows for small field-of-view detection, providing a higher order wavefront sensor. By the combination of the large-view-field low-order/small-view-field high-order shack-Hartmann wavefront sensor, different requirements of a traditional high-order adaptive optical system and a large-view-field surface layer adaptive optical system on a wavefront detector are met.
The image plane splitter is formed by combining a flat-top pyramid and a reflector. The device is mainly used for cutting a view field as required and guiding light rays of a specific view field to enter a corresponding wavefront sensor. The light rays of the off-axis field of view need to enter the corresponding wavefront detection channel by a reflector; the central field of view rays are transmitted directly into the corresponding wavefront sensor.
The relay optical path can be a single lens or a lens group, and is mainly used for constructing a new pupil surface position and matching the aperture and the position of the new pupil surface position with a subsequent micro lens array.
The micro lens array corresponds to the number of paths of the detection field, the central field detection micro lens array has small corresponding imaging field and more arrays, and the high-order wavefront detection of a small field can be realized; the peripheral field detection micro lens array has a large corresponding imaging field and a small number of arrays, and can realize large-field low-order wavefront detection.
The detection camera is a large-target-surface high-frame-frequency scientific grade CMOS camera or a CCD camera, is mainly used for receiving images focused by the micro-lens array and is used for subsequent correlation operation and wavefront aberration extraction.
Compared with the prior art, the invention has the following advantages:
(1) the invention aims at the ground surface wavefront detection requirement of the large-aperture foundation solar telescope with the ultra-large field of view, and carries out large-field multi-sight-line wavefront detection by taking a low-contrast expansion target as a beacon.
(2) The invention gives consideration to both large-field wavefront detection and high-order wavefront detection, can simultaneously meet the requirements of the traditional high-order AO and large-field GLAO wavefront detection, and solves the problem that the large-field wavefront sensor needs an auxiliary device to measure the transfer function of a control system in the traditional scheme.
(3) The invention can obtain more wave-front detection information in the sight direction under the condition of a limited wave-front detection channel, and is more beneficial to extracting the turbulence information of the surface layer.
(4) Based on the integrated view field cutting module, the light path structure is simplified, error sources are reduced, and the system application cost and complexity are reduced.
In a word, compared with the traditional large-view-field wavefront sensor, the invention breaks through the problem that the detection view field/detection order is limited by the detection camera technology, has larger detection view field and meets the requirement of the large-caliber solar telescope GLAO detection view field. Meanwhile, large-field wave-front detection and high-order wave-front detection are considered, and the measurement of a system control system transfer function and the closed-loop capability of the traditional AO diffraction limit are realized; compared with the current scheme of cutting the wavefront sensor of the focal plane, the method can provide more wavefront information of the detection view field under the condition of cutting the same number of the detection view fields; meanwhile, the flat-top pyramid is used as a view field segmentation device, so that the design of the wavefront sensor is simplified, and the method is more economical and easier to realize.
Drawings
FIG. 1 is a schematic view of the apparatus according to the present invention;
FIG. 2 is a schematic diagram of a structural layout of an embodiment of the present invention;
FIG. 3 is a view of field segmentation for an embodiment of the present invention;
figure 4 is a diagram of the sub-aperture layout of an on-axis and off-axis wavefront sensor according to one embodiment of the present invention.
The reference numbers in the figures mean: the system comprises an image plane splitter 1, a flat pyramid 11, a reflecting mirror 12, a relay light path 2, a micro lens array 3 and a detection camera 4.
Detailed Description
The present invention will be described in detail below with reference to the accompanying drawings and specific embodiments.
As shown in fig. 1, the large-field-of-view high-order composite wavefront sensor for solar adaptive optics of the present invention includes an image plane splitter 1, a relay optical path 2, a micro lens array 3 and a corresponding detection camera 4; the image plane divider 1 divides an image plane and then guides the image plane into different detection channels, each detection channel comprises a relay light path 2, a micro lens array 3 and a detection camera 4, and wavefront detection is carried out on a specific view field. After the image plane splitter divides the focal plane of the telescope, the focal plane of the telescope is respectively guided to enter different detection channels; wherein, the on-axis detection channel corresponds to a dozen angular seconds detection field of view, and the off-axis detection channel corresponds to an angularly graded detection field of view. A large-view-field wavefront sensor is arranged on the off-axis detection channel, and detection information in different sight directions can be obtained by selecting different sub-regions of the sub-aperture image. Therefore, under the condition of the same detection channel, more accumulated wavefront aberrations of the detection field of view can be obtained; the on-axis channel only allows for small field-of-view detection, providing a higher order wavefront sensor. By the combination of the large-view-field low-order/small-view-field high-order shack-Hartmann wavefront sensor, different requirements of a traditional high-order adaptive optical system and a large-view-field surface layer adaptive optical system on a wavefront detector are met.
The image plane splitter 1 is formed by combining a flat-top pyramid and a reflector. The device is mainly used for cutting a view field as required and guiding light rays of a specific view field to enter a corresponding wavefront sensor. The light rays of the off-axis field of view need to enter the corresponding wavefront detection channel by a reflector; the central field of view rays are transmitted directly into the corresponding wavefront sensor.
The relay optical path 2 may be a single lens or a lens group, and is mainly used for constructing a new pupil surface position and matching the aperture and position with a subsequent microlens array.
The micro lens array 3 corresponds to the number of paths of the detection field, the central field detection micro lens array has small corresponding imaging field and more arrays, and the high-order wavefront detection of a small field can be realized; the peripheral field detection micro lens array has a large corresponding imaging field and a small number of arrays, and can realize large-field low-order wavefront detection.
The detection camera 4 is a large-target-surface high-frame-frequency scientific grade CMOS camera or a CCD camera, and is mainly used for receiving images focused by the micro-lens array and used for subsequent correlation operation and wavefront aberration extraction.
Fig. 2 to 4 show a specific design example based on the inventive concept of the present invention. The embodiment is based on a solar telescope with the aperture of 1.8 meters, wherein fig. 2 is a schematic structural layout diagram of a large-view-field high-order composite wavefront sensor, and fig. 3 is a schematic structural layout diagram of a view field which is divided by an image plane divider and enters each detection channel and a schematic structural layout diagram of a detection view field corresponding to each wavefront sensor. FIG. 4 is a layout of a microlens array for on-axis and off-axis fields of view.
In fig. 2, light from the telescope forms an image-wise telecentric optical path, and the focal plane of the telescope is located at the position of the flat-top pyramid 11. The flat-top pyramid 11 and the reflector 12 jointly form a focal plane splitter, so that light rays in different view fields are split and guided to enter different detection channels, and the system can change the widths of the flat-top pyramid, the flat top and the inclined plane according to detection requirements and adjust the view fields of different detection channels. In the example, a flat-top rectangular pyramid is used to divide the telescope focal plane into 5 regions (the other two detection channels are not shown), for example, the detection channel 2 corresponds to the central field of view and only passes through the field of view for 20 seconds, and the off-axis fields of view are respectively introduced into the four surrounding detection channels, which correspond to the large field of view detection. Each detection channel comprises a relay light path 2, a micro lens array 3 and a detection camera 4. The relay optical path 2 constructs a proper pupil surface position and aperture to match with a subsequent micro-lens array. And meanwhile, a focal plane position is reserved for placing a field diaphragm. As can be seen from fig. 3, in this example, the telescope field of view is divided into 5 angular divisions (300 arc seconds), after the field of view is divided, the on-axis detection channel corresponds to the 20 arc second field of view for high-order detection, the off-axis detection channel corresponds to the 1 angular division field of view, and in each detection channel, 5 sight directions can be selected as needed for wavefront detection. That is, 5 imaging channels can achieve wavefront detection of 21 line-of-sight directions.
FIG. 4 is a layout of a microlens array for on-axis and off-axis fields of view. Aiming at a telescope with the caliber of 1.8 meters, in order to ensure the wavefront detection capability of enough high order, the small-field high-order shack-Hartmann wavefront sensor needs at least 23 multiplied by 23 sub-apertures, the corresponding space sampling scale is about 8cm, and effective high-precision detection on medium atmospheric seeing can be ensured. The pixel resolution of the wave-front sensor is 0.6 arcsec/pixel calculation, a field of view is detected within 15 seconds, a single sub-aperture corresponds to 25 pixels, the target surface of the high-order wave-front sensor needs to reach about 825 multiplied by 825, and the current SCMOS camera can meet the sampling frequency of kilohertz on the wave-front sensor. For the off-axis detection channel, to ensure that the wavefront sensor detects a field of view for 60 seconds, and the sampling rate of 0.6 arc seconds/pixel, a single sub-aperture corresponds to 100 pixels, and the sub-aperture layout of 11 × 11 requires that the target surface of the camera has reached 1100 × 1100, which is the technical limit of the current detection camera.
Parts of the invention not described in detail are well known in the art.
Claims (5)
1. A large-field-of-view high-order composite wavefront sensor for solar adaptive optics, characterized by: the device comprises an image plane divider (1), a relay light path (2), a micro lens array (3) and a corresponding detection camera (4); the image plane divider (1) divides an image plane and then guides the divided image plane into different detection channels, each detection channel comprises a relay light path (2), a micro lens array (3) and a detection camera (4), and wavefront detection is carried out on a specific view field; the image plane divider (1) divides the focal plane of the telescope and guides the focal plane of the telescope into different detection channels; wherein, the on-axis detection channel corresponds to a dozen angular seconds detection field of view, and the off-axis detection channel corresponds to an angular grading detection field of view; the method comprises the steps that a large-field-of-view wavefront sensor is arranged on an off-axis detection channel, detection information in different sight directions can be obtained by selecting different sub-regions of a sub-aperture image, and more accumulated wavefront aberrations of detection fields can be obtained under the condition of the same detection channel; the on-axis channel only considers the detection of a small visual field and is provided with a high-order wavefront sensor; by the combination of the large-view-field low-order/small-view-field high-order shack-Hartmann wavefront sensor, different requirements of a traditional high-order adaptive optical system and a large-view-field surface layer adaptive optical system on a wavefront detector are met.
2. The large-field high-order composite wavefront sensor for solar adaptive optics is characterized in that an image plane divider (1) is formed by combining a flat-top pyramid (11) and a reflector (12) and is mainly used for cutting a field of view as required and guiding light rays of a specific field of view to enter a corresponding wavefront sensor, wherein light rays of a central field of view directly penetrate into the corresponding wavefront sensor, and light rays of an off-axis field of view enter a corresponding wavefront detection channel with the aid of the reflector.
3. A large field of view high order compound wavefront sensor for solar adaptive optics according to claim 1 where the relay optical path (2) can be a single lens or a set of lenses primarily used to construct new pupil surface locations and match their aperture and location to the subsequent microlens array.
4. The large-view-field high-order composite wavefront sensor for solar adaptive optics is characterized in that the number of paths of the micro lens array (3) corresponds to the number of paths of a detection view field, wherein the central view field detection micro lens array has a small imaging view field and a large array number, and can realize small-view-field high-order wavefront detection; the imaging field of view of the peripheral field-of-view detection micro-lens array is large, the number of the array is small, and large-field-of-view low-order wavefront detection can be realized.
5. The large field of view high order compound wavefront sensor for solar adaptive optics according to claim 1, characterized by the detection camera (4) being a large target surface high frame rate scientific grade CMOS camera or CCD camera, primarily intended to receive the micro lens array focused image for subsequent correlation and extraction of wavefront aberrations.
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