A pupil-adaptive optical path adjustment method

Abstract

This invention discloses a pupil-adaptive optical path adjustment method, comprising: inserting two optical path adjustment boxes into the optical paths of corresponding sub-telescopes of a beam combiner telescope; adjusting the positions of the sub-telescopes and the beam combiner telescope according to the detection baseline requirements of the space distributed optical synthetic aperture detection system; adjusting the pointing adjustment mirror of the beam combiner telescope so that the beam combiner telescope can receive the observation beam from the sub-telescopes; adjusting the relative pointing of the sub-telescopes to keep them within the required deviation range; moving the optical path adjustment boxes to perform large optical path adjustment, adjusting the optical path difference between the sub-telescopes to the micrometer level; using the integrated adjuster in the optical path adjustment boxes to perform small optical path and tilt adjustments, so that the optical path and pointing between the sub-telescopes are consistent; and adjusting the exit pupil position of the space distributed optical synthetic aperture detection system through the curvature adjustment function of the integrated adjuster in the optical path adjustment boxes, so that the exit pupil position of the system does not change due to changes in optical path, thus completing the pupil-adaptive optical path adjustment.

Description

Technical Field

[0001] This invention relates to a pupil-adaptive optical path adjustment method, which can be used to adjust the optical path difference between sub-apertures while keeping the exit pupil position of the system unchanged, and belongs to the field of distributed optical synthetic aperture detection. Background Technology

[0002] Space-distributed optical synthetic aperture (OSA) systems typically utilize multiple telescopes arranged over a long distance, collecting light from each telescope for co-phase interference. Their spatial resolution is equivalent to the spatial resolution corresponding to the maximum outer envelope aperture of the multiple telescopes, thus reducing the difficulty and cost of developing ultra-large aperture telescopes. The sub-telescopes in a space-distributed OSA system are approximately several meters in size. Due to the limited size of the beam combiner, multiple stages of optical beam compression are required to reduce the beam size to the tens of millimeters. To achieve equivalent maximum outer envelope aperture detection, pointing mirrors are needed to ensure consistent optical path pointing of each sub-telescope, and the optical path lengths of the two sub-aperture beams used for beam combining must be adjusted to a nanometer-level difference before beam combining and interference detection.

[0003] For space-distributed optical synthetic aperture detectors (OSAPs) used to search for habitable exoplanets, nullification interferometry is required. In addition to meeting the above requirements, the detector must be placed at the exit pupil of the optical system to eliminate the bright starlight on the axis to the maximum extent, so as to better obtain faint planetary information. The more starlight is eliminated, the greater the nullification depth of the system and the better the planetary information detection effect.

[0004] The traditional method uses separate multi-stage optical beam compression modules, compressing the optical beam at different locations to a size that the beam combiner telescope can handle. The beam combiner telescope then adjusts the optical path length of each sub-path by changing the distance between the two sets of roof mirrors. When the exit pupil position changes, the detector position is adjusted to adapt to the change in exit pupil position, thereby obtaining optimal detection data. However, this method mainly has the following problems:

[0005] (1) This system includes optical beam compression module, optical path adjustment module and detector adjustment mechanism, etc. There are many optical components and the optical link is complex. Therefore, the number of system error sources increases, which makes it difficult for the space distributed optical synthetic aperture detection system to achieve high-precision stable interference in orbit.

[0006] (2) It cannot automatically compensate for changes in exit pupil position caused by optical path adjustment. When the sub-aperture distance changes significantly, the exit pupil position also changes significantly. Due to the limited size and volume of space telescopes, the detection method of adjusting the detector position to adapt to changes in exit pupil position cannot be engineered on space telescopes. Summary of the Invention

[0007] The technical problem solved by this invention is to overcome the shortcomings of the prior art and provide a pupil-adaptive optical path adjustment method, which reduces the required optical mirrors, simplifies the composition of the optical system, eliminates the change in the exit pupil position caused by the change in optical path, compensates for the optical axis pointing deviation caused by the optical path adjustment process, improves the zero-shaving depth, and ensures system performance.

[0008] The technical solution of this invention is: a pupil-plane adaptive optical path adjustment method, comprising:

[0009] Two optical path adjustment boxes are respectively inserted into the optical paths of the corresponding sub-telescopes of the beam combiner telescope in the space distributed optical synthetic aperture detection system; the optical path adjustment boxes are equipped with optical elements and integrated adjustment devices.

[0010] Adjust the positions of the sub-telescopes and the combined telescope according to the detection baseline requirements of the space distributed optical synthetic aperture detection system, so that the stars in the observed star-planet system are located in the central field of view of each sub-telescope, and maintain this observation configuration after the adjustment is completed.

[0011] Adjust the pointing adjustment mirror of the beam combiner telescope so that it can receive the observation beam from the sub-telescope; adjust the relative pointing of the two sub-telescopes so that their relative pointing is within the required deviation range.

[0012] The movable optical path adjustment box is used to adjust the optical path difference between the sub-telescopes to the micrometer level.

[0013] Use the integrated adjuster in the optical path adjustment box to make small optical path and tilt adjustments so that the optical path and pointing of the sub-telescopes are consistent.

[0014] Adjusting the curvature of the integrated adjuster in the optical path adjustment box adjusts the exit pupil position of the spatially distributed optical synthetic aperture detection system, ensuring that the exit pupil position does not change due to changes in optical path, thus achieving adaptive optical path adjustment of the pupil surface.

[0015] Preferably, two through holes are provided on one end face of the optical path adjustment box, for light input and light output respectively, and this end face is defined as the light input / output surface; the optical path adjustment box is equipped with optical elements and a comprehensive adjustment device, specifically:

[0016] The three optical elements include a primary mirror, a secondary mirror, and a tertiary mirror. The optical axes of all three optical elements are parallel to the light-incident and light-excising surfaces of the optical path adjustment box, and they are placed inside the optical path adjustment box with their optical centers on the same straight line. The primary mirror is a parabolic mirror, located between the secondary and tertiary mirrors. The secondary mirror is a hyperboloid mirror, located on the inner wall between the light-incident and light-excising apertures. The tertiary mirror is a curvature-adjustable mirror, integrated with the integrated adjustment unit, and located at the focal point of the secondary mirror.

[0017] The integrated adjuster can adjust the displacement of the three mirrors to achieve nanometer-level small optical path adjustment, and can also adjust the tilt and curvature of the three mirrors.

[0018] Preferably, the outgoing light from the sub-telescope enters the beam combiner telescope, which includes a pointing adjustment mirror, a beam compressor, an optical path adjustment box, a pointing detection unit, a null detection unit, a phase coarse detection unit, and a phase fine detection unit; specifically:

[0019] The optical path of each sub-telescope is adjusted by the pointing adjustment mirror of the beam combiner and then compressed by the beam compressor. The compressed light enters the optical path adjustment box for optical path adjustment. The light emitted from the optical path adjustment box is split into three beams. One beam is used for pointing detection in the pointing detection unit. Another beam is used for phase coarse detection in the phase coarse detection unit after dispersion with the beam corresponding to another sub-telescope. The last beam is also coaxially combined with the beam corresponding to another sub-telescope and then split into two beams. One beam is used for phase fine detection in the phase fine detection unit, and the other beam is used for zero-elimination detection in the zero-elimination detection unit.

[0020] Preferably, the relative pointing of the two sub-telescopes is adjusted to keep them within the required deviation range. Specifically, this involves: obtaining pointing detection data through centroid detection, analyzing the relative pointing deviation of each sub-telescope from the data, and rotating the pointing adjustment mirror of the beam combiner telescope according to the relative pointing deviation; repeating the above process until the relative pointing of the sub-telescopes is kept within the required deviation range.

[0021] Preferably, when the moving optical path adjustment box is used for large optical path adjustment:

[0022] In the phase coarse detection unit, phase coarse detection is carried out between sub-telescopes using two-dimensional dispersion fringe detection technology. The optical path difference of the sub-telescopes is identified using two-dimensional dispersion fringe analysis technology. Using this optical path difference information as input, the optical path difference is adjusted with micron-level precision by moving the optical path adjuster. The above process is repeated for real-time closed-loop measurement and control until the optical path difference of the sub-telescopes is less than λ / 4, where λ is the center wavelength of the phase coarse detection.

[0023] Preferably, when the integrated adjuster in the optical path adjustment box performs small optical path and tilt adjustments:

[0024] In the phase fine detection unit, phase fine detection is carried out between the sub-telescopes using pupil plane interferometry detection technology. The optical path difference information when the light from the two sub-telescopes reaches the null detection unit of the beam combiner telescope is obtained in real time. This optical path difference information is used as input to drive the integrated adjuster to translate so that the optical path difference is less than λ1 / 20, where λ1 is the center wavelength of the phase fine detection. At the same time, the relative pointing deviation of the sub-telescopes drives the piezoelectric ceramic tilting mirror inside the integrated adjuster to compensate for the tilt deviation caused by the optical path adjustment, so that the optical path and pointing between the sub-telescopes are consistent.

[0025] Preferably, when adjusting the curvature of the integrated adjuster in the optical path adjustment box:

[0026] First, based on the range of optical path change, the piezoelectric ceramic inside the integrated adjuster is driven to coarsely adjust the curvature of the three mirrors. Then, zero-elimination detection is performed through the zero-elimination detection unit. Based on the zero-elimination depth calculated in real time during the zero-elimination detection, the piezoelectric ceramic inside the integrated adjuster is driven again to finely adjust the curvature of the three mirrors. The above process is repeated until the change in zero-elimination depth tends to stabilize, thus completing the exit pupil position adjustment.

[0027] Preferably, the relative pointing deviation range of the sub-telescope is ±0.01″.

[0028] Compared with the prior art, the present invention has the following advantages:

[0029] (1) This method does not require setting up a detector position adjustment function, and does not need to consider the problem that the corresponding detector adjustment space is insufficient and normal detection cannot be achieved when adjusting the optical path is large. The use of this method can meet the availability of the system when adjusting the optical path is large.

[0030] (2) This method replaces the roof mirror group to achieve optical path adjustment, without having to consider the back reflection accuracy of the roof mirror group, and can realize the function of motion tilt compensation that the roof mirror group cannot perform in optical path adjustment, thereby reducing error sources and improving optical accuracy.

[0031] (3) This method adjusts the curvature of the three mirrors by piezoelectric ceramics. It is simple and reliable, and can adapt to the optical path adjustment to restore the exit pupil position, thus improving the system's flexibility and spatial adaptability. Attached Figure Description

[0032] Figure 1 This is a schematic diagram of the beam combining of the sub-telescopes of the present invention;

[0033] Figure 2 This is a schematic diagram of the optical path adjustment box for the optical path adjustment method for pupil-plane adaptive optical path adjustment of the present invention;

[0034] Figure 3 This is the optical path diagram of the optical path adjustment box of the present invention;

[0035] Figure 4 The following is a simulation diagram of the pupil-plane adaptive optical path adjustment process according to an embodiment of the present invention, wherein (a) is a simulation diagram of the initial state of the optical system, (b) is a simulation diagram of the large optical path adjustment, (c) is a simulation diagram of the optical path adjustment box tilted by 0.02 degrees, (d) is a simulation diagram of the curvature adjustment of the three mirrors, and (e) is a simulation diagram of the position of the outgoing light and the position of the exit pupil after the tilt adjustment of the three mirrors. Detailed Implementation

[0036] The technical solution of this invention is: a pupil-plane adaptive optical path adjustment method in a space-distributed optical synthetic aperture detection system, mainly comprising three optical elements (primary mirror, secondary mirror, and tertiary mirror) and a set of small optical path, curvature, and tilt integrated adjusters, with the connection relationship as follows: Figure 2 As shown, two through holes are provided on one end face of the optical path adjustment box, used for light input and light output respectively, and this end face is defined as the light input / output surface. The optical axes of the three optical elements are all parallel to the light input / output surface of the optical path adjustment box and are placed inside the optical path adjustment box, with their optical centers on the same straight line. The primary mirror is a parabolic mirror, located between the secondary and tertiary mirrors. The secondary mirror is a hyperboloid mirror, located on the inner wall between the light input and output apertures. The tertiary mirror is a curvature-adjustable mirror. The three optical elements are installed in the optical path adjustment box according to preset optical positions, with the tertiary mirror located at the focal point of the secondary mirror. The optical path adjustment box is located on a linear translation guide rail designed for large optical path adjustment. The entire module can achieve a wide range of optical path adjustment through the back-and-forth movement of the linear translation guide rail, with an optical path adjustment accuracy down to the micrometer level, driven by a DC motor. The three mirrors are integrated with a small optical path, curvature, and tilt adjustment device. This device achieves nanometer-level fine optical path adjustment through the displacement of piezoelectric ceramic devices; it adjusts the tilt of the three mirrors through the displacement difference of multiple piezoelectric ceramic devices, compensating for tilt errors that may be introduced during the mechanical movement of the optical path adjustment box; and it also adjusts the curvature of the three mirrors through piezoelectric ceramic devices, compensating for changes in the exit pupil position of the optical system caused by changes in optical path. Therefore, by inserting the optical path adjustment box used in this method into the corresponding sub-telescope optical path of the beam combiner telescope in a space distributed optical synthetic aperture detection system, three optical elements can be used to achieve five reflections, allowing the sub-telescope optical system to re-image at the original exit pupil position even after changes in optical path, ensuring the zero-elimination depth of the co-phase interference imaging, and making the space distributed optical synthetic aperture detection mission feasible.

[0037] The output light from the sub-telescope enters the beam combiner telescope, which includes a pointing adjustment mirror, a beam compressor, an optical path adjustment box, a pointing detection unit, a nulling detection unit, a phase coarse detection unit, and a phase fine detection unit; specifically:

[0038] The optical path of each sub-telescope is adjusted by the pointing adjustment mirror of the beam combiner and then compressed by the beam compressor. The compressed light enters the optical path adjustment box for optical path adjustment. The light emitted from the optical path adjustment box is split into three beams. One beam is used for pointing detection in the pointing detection unit. Another beam is used for phase coarse detection in the phase coarse detection unit after dispersion with the beam corresponding to another sub-telescope. The last beam is also coaxially combined with the beam corresponding to another sub-telescope and then split into two beams. One beam is used for phase fine detection in the phase fine detection unit, and the other beam is used for zero-elimination detection in the zero-elimination detection unit.

[0039] The pupil-adaptive optical path adjustment method specifically includes the following steps:

[0040] (1) Adjust the position and attitude of the sub-telescopes and the combined telescope. Adjust the position of the sub-telescopes and the combined telescope according to the detection baseline of the space distributed optical synthetic aperture detection system (the baseline is the distance between the sub-telescopes). The attitude adjustment goal is to place the stars in the observed star-planet system in the central field of view of each sub-telescope, and maintain the aforementioned observation configuration of the combined telescope and the sub-telescopes.

[0041] (2) Adjust the pointing adjustment mirror of the beam combiner telescope so that the beam combiner telescope can receive the observation beam from the sub-telescopes. Obtain pointing detection data through centroid detection, analyze the relative pointing deviation of each sub-telescope, and rotate the pointing adjustment mirror to ensure that the relative pointing of the sub-telescopes is kept within the required deviation range.

[0042] (3) Large optical path adjustment is performed through the optical path adjustment box to adjust the optical path difference between the sub-telescopes to the micrometer level. In the phase coarse detection unit, phase coarse detection is carried out between the sub-telescopes using two-dimensional dispersion fringe detection technology. The optical path difference between the sub-telescopes is identified using two-dimensional dispersion fringe analysis technology. The micrometer-level precision optical path difference is adjusted by the movement of the optical path adjuster on the guide rail. This measurement-adjustment form a real-time closed-loop measurement and control until the optical path difference is less than λ / 4 (λ is the center wavelength of the phase coarse detection).

[0043] (4) The optical path and pointing consistency of the sub-telescopes are adjusted by using the small optical path and tilt adjustment functions of the integrated adjuster in the optical path adjustment box. In the phase fine detection unit, the phase fine detection between the sub-telescopes is carried out by the pupil plane interferometry detection technology to obtain the optical path difference information when the two sub-telescopes reach the zero-clearing detection unit position in real time. This information is used as input to drive the piezoelectric ceramic inside the integrated adjuster so that the optical path difference is less than λ1 / 20 (λ1 is the center wavelength of the phase fine detection). At the same time, the relative pointing deviation information obtained by combining the phase fine detection with the pointing detection is used to drive the piezoelectric ceramic tilting mirror inside the integrated adjuster to compensate for the tilt deviation caused by the optical path adjustment, thereby achieving the consistency of optical path and pointing between the sub-telescopes.

[0044] (5) The exit pupil position of the spatially distributed optical synthetic aperture detection system is adjusted by the curvature adjustment function of the integrated adjuster in the optical path adjustment box, so that the exit pupil position does not change due to changes in optical path. Changes in optical path will cause changes in the exit pupil position. Detection away from the exit pupil position will lead to a decrease in the zero-elimination depth in the zero-elimination detection. First, based on the range of optical path change, the curvature of the three mirrors is coarsely adjusted by driving the piezoelectric ceramic inside the integrated adjuster. Zero-elimination detection is then performed by the zero-elimination detection unit. Then, based on the zero-elimination depth calculated in real time during the zero-elimination detection, the piezoelectric ceramic inside the integrated adjuster is driven again to finely adjust the curvature of the three mirrors until the change in zero-elimination depth tends to stabilize, at which point the exit pupil position adjustment is considered complete.

[0045] Example:

[0046] The specific steps are as follows:

[0047] (1) Adjust the position and attitude of the sub-telescopes and the combined telescope. Adjust the position of the sub-telescopes and the combined telescope according to the detection baseline of the space distributed optical synthetic aperture detection system (the baseline is the distance between the sub-telescopes). The attitude adjustment goal is to make the stars in the observed star-planetary system located in the central field of view of each sub-telescope, and to maintain the observation configuration of the combined telescope and the sub-telescopes.

[0048] (2) Adjust the pointing adjustment mirror of the beam combiner telescope so that it can receive the observation beams from the sub-telescopes. Analyze the relative pointing deviation of each sub-telescope using pointing detection data and phase detection data. Rotate the pointing adjustment mirror to ensure that the relative pointing of the sub-telescopes remains within the required deviation range. Define this state as the initial state. Figure 4 As shown in (a), the exit pupil position of the system is -25274.35 at this time, and the position coordinates of the emitted ray are shown in the figure.

[0049] (3) Perform coarse phase detection and use two-dimensional dispersive fringe analysis to identify the optical path difference of the sub-telescope. Assuming the current optical path difference is 100mm, by moving the guide rail on the large optical path adjuster, the optical path adjustment box is moved 100mm to the right, resulting in an actual optical path change of 200mm. At this time, the exit pupil position changes to -25074.32. Figure 4 As shown in (b), there is a deviation of about 200 mm from the initial state, and the position coordinates of the emitted ray are shown in the figure.

[0050] (4) Assume that during the large optical path adjustment, the optical path adjustment box tilts by an angle of 0.02 degrees around the x-axis. Figure 4 As shown in (c), the exit pupil position changes to -25077.03, and the emitted beam is translated. As shown in the figure, the Y coordinate is translated to -1.199906004E+02.

[0051] (5) Using the curvature adjustment function of the integrated adjuster in the optical path adjustment box, adjust the curvature of the three mirrors to 1.6223E+05, as shown. Figure 4 As shown in (d), the exit pupil position returns to the initial position of -25274.35, but the Y-direction offset of the emitted beam still exists.

[0052] (6) Adjust the three-mirror deflection angle, rotating it around the Y-axis by -0.000765 degrees, as shown. Figure 4 As shown in (e), the outgoing beam is deflected and adjusted in the Y direction to return to the initial state, and the exit pupil position remains unchanged.

[0053] At this point, the optical path adjustment box has completed the optical path adjustment while maintaining the original exit pupil position, and the beam has not shifted.

[0054] The contents not described in detail in this specification are existing technologies known to those skilled in the art.

Claims

1. A pupil-plane adaptive optical path adjustment method, characterized in that... include: Insert the two optical path adjustment boxes into the corresponding sub-telescope optical paths of the beam combiner telescope in the space distributed optical synthetic aperture detection system; The optical path adjustment box contains optical elements and a comprehensive adjuster. Two through holes are located on one end face of the box, used for light input and output respectively; this end face is defined as the light input / output surface. Specifically, the three optical elements include a primary mirror, a secondary mirror, and a tertiary mirror. The optical axes of all three optical elements are parallel to the light input / output surface of the optical path adjustment box and are placed inside the box, with their optical centers on the same straight line. The primary mirror is a parabolic mirror located between the secondary and tertiary mirrors. The secondary mirror is a hyperboloid mirror located on the inner wall between the light input and output apertures. The tertiary mirror is a curvature-adjustable mirror, integrated with the comprehensive adjuster, and located at the focal point of the secondary mirror. The comprehensive adjuster can adjust the displacement of the tertiary mirrors to achieve nanometer-level small optical path adjustment, and can also adjust the tilt and curvature of the tertiary mirrors. The light emitted from the sub-telescopes enters the beam combiner, which includes a pointing adjustment mirror, a beam compressor, an optical path adjustment box, a pointing detection unit, a null detection unit, a phase coarse detection unit, and a phase fine detection unit. Specifically: the light path of each sub-telescope is adjusted by the pointing adjustment mirror of the beam combiner and then compressed by the beam compressor. The compressed light enters the optical path adjustment box for optical path adjustment. The light emitted from the optical path adjustment box is split into three beams. One beam is used for pointing detection in the pointing detection unit. Another beam is used for phase coarse detection in the phase coarse detection unit after dispersion with the beam corresponding to another sub-telescope. The last beam is also used for coaxial combination with the beam corresponding to another sub-telescope and then split into two beams. One beam is used for phase fine detection in the phase fine detection unit, and the other is used for null detection in the null detection unit. Adjust the positions of the sub-telescopes and the combined telescope according to the detection baseline requirements of the space distributed optical synthetic aperture detection system, so that the stars in the observed star-planet system are located in the central field of view of each sub-telescope to form an observation configuration, and maintain this observation configuration after the adjustment is completed. Adjust the pointing adjustment mirror of the beam combiner telescope so that it can receive the observation beam from the sub-telescope; adjust the relative pointing of the two sub-telescopes so that their relative pointing is within the required deviation range. The movable optical path adjustment box is used to adjust the optical path difference between the sub-telescopes to the micrometer level. Use the integrated adjuster in the optical path adjustment box to make small optical path and tilt adjustments so that the optical path and pointing of the sub-telescopes are consistent. Adjust the curvature of the three mirrors in the optical path adjustment box, and adjust the exit pupil position of the spatially distributed optical synthetic aperture detection system so that the exit pupil position does not change due to changes in optical path, thus completing the pupil-plane adaptive optical path adjustment.

2. The pupil-plane adaptive optical path adjustment method according to claim 1, characterized in that: Adjust the relative pointing of the two sub-telescopes to keep them within the required deviation range. Specifically, obtain pointing detection data through centroid detection, analyze the relative pointing deviation of each sub-telescope from it, and rotate the pointing adjustment mirror of the beam combiner telescope according to the relative pointing deviation. Repeat the above process until the relative pointing of the sub-telescopes is kept within the required deviation range.

3. The pupil-plane adaptive optical path adjustment method according to claim 1, characterized in that: When the moving optical path adjustment box is used for large optical path adjustment: In the phase coarse detection unit, phase coarse detection is carried out between sub-telescopes using two-dimensional dispersion fringe detection technology. The optical path difference of the sub-telescopes is identified using two-dimensional dispersion fringe analysis technology. Using this optical path difference information as input, the optical path difference is adjusted with micron-level precision by moving the optical path adjuster. The above process is repeated for real-time closed-loop measurement and control until the optical path difference of the sub-telescopes is less than λ / 4, where λ is the center wavelength of the phase coarse detection.

4. The pupil-plane adaptive optical path adjustment method according to claim 1, characterized in that: When the integrated adjuster in the optical path adjustment box is used for small optical path and tilt adjustments: In the phase fine detection unit, phase fine detection is carried out between the sub-telescopes using pupil plane interferometry detection technology. The optical path difference information when the light from the two sub-telescopes reaches the null detection unit of the beam combiner telescope is obtained in real time. This optical path difference information is used as input to drive the integrated adjuster to translate so that the optical path difference is less than λ1 / 20, where λ1 is the center wavelength of the phase fine detection. At the same time, the relative pointing deviation of the sub-telescopes drives the piezoelectric ceramic tilting mirror inside the integrated adjuster to compensate for the tilt deviation caused by the optical path adjustment, so that the optical path and pointing between the sub-telescopes are consistent.

5. The pupil-plane adaptive optical path adjustment method according to claim 1, characterized in that: When adjusting the curvature of the three mirrors in the optical path adjustment box: First, based on the range of optical path change, the piezoelectric ceramic inside the integrated adjuster is driven to coarsely adjust the curvature of the three mirrors. Then, zero-elimination detection is performed through the zero-elimination detection unit. Based on the zero-elimination depth calculated in real time during the zero-elimination detection, the piezoelectric ceramic inside the integrated adjuster is driven again to finely adjust the curvature of the three mirrors. The above process is repeated until the change in zero-elimination depth tends to stabilize, thus completing the exit pupil position adjustment.

6. The pupil-plane adaptive optical path adjustment method according to claim 2, characterized in that: The relative pointing deviation range of the sub-telescope is ±0.01″.

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