Pupil plane self-adaptive optical path adjustment method

Abstract

The invention discloses a pupil plane self-adaptive optical path adjusting method. The method comprises the following steps: respectively inserting two optical path adjusting boxes into corresponding sub-telescope optical paths of a beam combining telescope; adjusting the positions of the sub-telescope and the beam-combining telescope according to the detection baseline requirement of the spatial distributed optical synthetic aperture detection system; adjusting a pointing adjusting mirror of the beam-combining telescope to enable the beam-combining telescope to receive the observation light beams from the sub-telescopes; adjusting the relative direction of the sub-telescope, and keeping the relative direction in a required deviation range; an optical path adjusting box is moved to carry out large optical path adjustment, and the optical path difference between the sub-telescopes is adjusted to a micron order; a comprehensive adjuster in the optical path adjusting box is used for small optical path and inclination adjustment, so that the optical paths and directions of the sub-telescopes are consistent; the exit pupil position of the spatial distributed optical synthetic aperture detection system is adjusted through the curvature adjusting function of a comprehensive adjuster in the optical path adjusting box, so that the exit pupil position of the system does not change along with the change of the optical path, and the self-adaptive optical path adjustment of the pupil plane is completed.

Description

Technical Field

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

[0002] The spatially distributed optical synthetic aperture detection system usually uses multiple telescopes arranged at a long distance and collects the light from each telescope for common phase interference. Its spatial resolution is equivalent to the spatial resolution corresponding to the maximum outer envelope aperture of multiple telescopes, thereby reducing the difficulty of developing ultra-large aperture telescopes and reducing costs. The size of the sub-telescopes in the spatially distributed optical synthetic aperture detection system is about several meters. Due to the limited size of the beam combining telescope, it is necessary to perform multi-stage optical beam compression on the sub-telescope beam to reduce the beam size to ten millimeters. In order to achieve equivalent maximum outer envelope aperture detection, it is necessary to ensure that the optical path of each sub-telescope is consistent through a pointing adjustment mirror, and it is necessary to adjust the optical path of the two sub-aperture lights used for beam combining so that the optical path difference from the two sub-aperture lights is at the nanometer level before beam combining interference detection is performed.

[0003] For the spatially distributed optical synthetic aperture detection system for searching for habitable planets outside our solar system, since it is necessary to carry out zero-cancellation interferometry detection, in addition to meeting the above requirements, the detector must be placed at the exit pupil position of the optical system so that the bright starlight on the axis can be eliminated to the greatest depth, so as to better obtain the dim planetary information. The more starlight is eliminated, the greater the system zero-cancellation depth and the better the planetary information detection effect.

[0004] The traditional method is to use a separate multi-stage optical beam compression module to compress the optical beam to a size that the beam combining telescope can bear at different positions. In the beam combining telescope, the distance between the two groups of roof mirrors is changed to adjust the optical path of each sub-optical path. When the exit pupil position changes, the detector position is adjusted to adapt to the change of the exit pupil position, thereby obtaining the best detection data. However, this method has the following main problems:

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

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

[0007] The technical problem solved by the present invention is: to overcome the shortcomings of the prior art, to provide a pupil-plane adaptive optical path adjustment method, to reduce the required optical mirrors, to simplify the composition of the optical system, and at the same time to eliminate the change in the system exit pupil position caused by the change in the optical path, to compensate for the optical axis pointing deviation caused by the optical path adjustment process, to improve the zeroing depth, and to ensure the system performance.

[0008] The technical solution of the present 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 corresponding sub-telescopes of the beam combining telescope in the spatially distributed optical synthetic aperture detection system; wherein the optical path adjustment boxes are provided with optical elements and a comprehensive adjuster;

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

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

[0012] Move the optical path adjustment box to adjust the optical path difference between the sub-telescopes to micron level;

[0013] Use the integrated adjuster in the optical path adjustment box to adjust the small optical path and tilt to make the optical path and pointing direction of the sub-telescopes consistent;

[0014] The curvature of the integrated adjuster in the optical path adjustment box is adjusted to adjust the exit pupil position of the spatially distributed optical synthetic aperture detection system so that the exit pupil position of the system does not change due to the change of the optical path, thereby completing the pupil plane adaptive optical path adjustment.

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

[0016] The three optical elements include: a primary mirror, a secondary mirror, and a tertiary mirror; the optical axes of the three optical elements are parallel to the light entrance and exit surfaces of the optical path adjustment box and are placed in the optical path adjustment box, and the optical centers are on the same straight line; the primary mirror is a parabolic mirror, located between the secondary mirror and the tertiary mirror; the secondary mirror is a hyperbolic mirror, located on the inner wall between the light entrance hole and the light exit hole; the tertiary mirror is a curvature adjustable mirror, integrated with the integrated adjuster, and located at the focus 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 of the sub-telescope enters the beam combining telescope, which includes a pointing adjustment mirror, a beam compressor, an optical path adjustment box, a pointing detection unit, a zeroing detection unit, a coarse phase detection unit, and a fine phase detection unit; specifically:

[0019] The optical path of each telescope is adjusted in direction by the pointing adjustment mirror of the beam combining telescope 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 divided into three beams, one of which is subjected to pointing detection in the pointing detection unit, one is converged after being dispersed with the light beam corresponding to the other telescope in the coarse phase detection unit for coarse phase detection, and the last beam is also coaxially combined with the light beam corresponding to the other telescope, and then divided into two beams, one of which is subjected to fine phase detection in the fine phase detection unit, and the other is subjected to zeroing detection in the zeroing detection unit.

[0020] Preferably, the relative pointing of the two sub-telescopes is adjusted so as to remain within a required deviation range, specifically by: obtaining pointing detection data through centroid detection, parsing the relative pointing deviation of each sub-telescope therefrom, and rotating the pointing adjustment mirror of the beam combining telescope according to the relative pointing deviation; repeating the above process until the relative pointing of the sub-telescopes remains within the required deviation range.

[0021] Preferably, when moving the optical path adjustment box to adjust the large optical path:

[0022] In the coarse phase detection unit, coarse phase detection is carried out between the sub-telescopes through two-dimensional dispersion fringe detection technology, and the optical path difference of the sub-telescopes is identified using two-dimensional dispersion fringe analysis technology. The optical path difference information is used as input, and 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-telescope is less than λ / 4, where λ is the central wavelength of the coarse phase detection.

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

[0024] In the phase precision detection unit, the pupil interferometry detection technology is used to carry out phase precision detection between the sub-telescopes, and the optical path difference information when the light of the two sub-telescopes reaches the nulling detection unit of the beam combining telescope is obtained in real time. The 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 central wavelength of the phase precision detection. At the same time, the relative pointing deviation of the sub-telescope drives the piezoelectric ceramic tilt three mirrors inside the integrated adjuster to compensate for the tilt deviation caused by the optical path adjustment, so that the optical path and pointing direction between the sub-telescopes are consistent.

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

[0026] First, according to the range of optical path change, the piezoelectric ceramics inside the integrated adjuster are driven to coarsely adjust the curvature of the three mirrors, and zero detection is performed through the zero detection unit. According to the zero depth calculated in real time during the zero detection, the piezoelectric ceramics inside the integrated adjuster are driven again to fine-tune the curvature of the three mirrors. The above process is repeated until the zero depth change tends to be stable and the exit pupil position adjustment is completed.

[0027] Preferably, the deviation range required for the relative pointing of the sub-telescopes is: ±0.01″.

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

[0029] (1) This method does not require the detector position adjustment function to be set, and does not need to consider the problem of insufficient adjustment space for the corresponding detector during long optical path adjustment, which makes it impossible to achieve normal detection. The use of this method can meet the system availability during long optical path adjustment;

[0030] (2) This method replaces the roof mirror group to achieve optical path adjustment, without considering the retroreflection accuracy of the roof mirror group, and can achieve the function of motion tilt compensation that the roof mirror group cannot perform during optical path adjustment, thereby reducing error sources and improving optical accuracy;

[0031] (3) This method uses piezoelectric ceramics to adjust the curvature of the three mirrors. It is simple and reliable and can adaptively adjust the optical path to achieve the function of restoring the exit pupil position, thereby improving the flexibility and spatial adaptability of the system. BRIEF DESCRIPTION OF THE DRAWINGS

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

[0033] Figure 2 It is a schematic diagram of an optical path adjustment box for the optical path adjustment method for pupil surface self-adaptation of the present invention;

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

[0035] Figure 4 Schematic diagram of the simulation of the pupil-adaptive optical path adjustment process of an embodiment of the present invention, wherein (a) is a schematic diagram of the simulation of the initial state of the optical system, (b) is a schematic diagram of the simulation of the large optical path adjustment, (c) is a schematic diagram of the simulation of the optical path adjustment box tilted 0.02 degrees, (d) is a schematic diagram of the simulation of the curvature adjustment of the three mirrors, and (e) is a schematic diagram of the simulation of the position of the emergent light and the exit pupil position after the tilt adjustment of the three mirrors. DETAILED DESCRIPTION

[0036] The technical solution of the present invention is: a pupil plane adaptive optical path adjustment method in a spatially distributed optical synthetic aperture detection system, mainly including three optical elements (primary mirror, secondary mirror, and third mirror), a set of small optical path, curvature and tilt comprehensive adjusters, the connection relationship of which is as follows: Figure 2 As shown, two through holes are set on one end face of the optical path adjustment box, which are used for light entry and light exit respectively, and the end face is defined as the light entry and light exit surface; the optical axes of the three optical elements are placed in the optical path adjustment box parallel to the light entry and light exit surface of the optical path adjustment box, and the optical centers are on the same straight line; the primary mirror is a parabolic mirror, located between the secondary mirror and the third mirror; the secondary mirror is a hyperbolic mirror, located on the inner wall between the light entry hole and the light exit hole; the third mirror is a curvature adjustable mirror, and the three optical elements are installed in the optical path adjustment box according to the preset optical position, and the third mirror is located at the focus of the secondary mirror. The optical path adjustment box is located on a linear translation guide rail set for large optical path adjustment. The entire module can achieve a wide range of optical path adjustment through the forward and backward movement of the linear translation guide rail. The optical path adjustment accuracy reaches the micron level and is driven by a DC motor. The three mirrors are integrated with the small optical path, curvature and tilt integrated adjuster. The integrated adjuster realizes nanometer-level fine optical path adjustment through the displacement of piezoelectric ceramic devices; the tilt adjustment of the three mirrors is realized through the displacement difference of multiple piezoelectric ceramic devices, compensating for the tilt error that may be introduced during the mechanical movement of the optical path adjustment box; at the same time, the curvature of the three mirrors can be adjusted through the piezoelectric ceramic device to compensate for the change in the position of the exit pupil of the optical system caused by the change in the optical path. As described above, the optical path adjustment box used in this method is inserted into the optical path of the corresponding sub-telescope of the beam combining telescope in the spatially distributed optical synthetic aperture detection system. Three optical elements can be used, and after five reflections, the optical path of the sub-telescope optical system can still be re-imaged at the original exit pupil position after the optical path changes, ensuring the zeroing depth of the common phase interference imaging, making the spatially distributed optical synthetic aperture detection task feasible.

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

[0038] The optical path of each telescope is adjusted in direction by the pointing adjustment mirror of the beam combining telescope 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 divided into three beams, one of which is subjected to pointing detection in the pointing detection unit, one is converged after being dispersed with the light beam corresponding to the other telescope in the coarse phase detection unit for coarse phase detection, and the last beam is also coaxially combined with the light beam corresponding to the other telescope, and then divided into two beams, one of which is subjected to fine phase detection in the fine phase detection unit, and the other is subjected to zeroing detection in the zeroing detection unit.

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

[0040] (1) Adjust the position and attitude of the sub-telescopes and the beam-combining telescope. The positions of the sub-telescopes and the beam-combining telescope are adjusted according to the detection baseline of the spatially 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 star-planet system to be observed located in the central field of view of each sub-telescope. The beam-combining telescope and the sub-telescopes maintain the above-mentioned observation configuration.

[0041] (2) Adjust the pointing adjustment mirror of the beam combining telescope so that the beam combining telescope can receive the observation beam from the sub-telescopes. Obtain the pointing detection data through the center of mass 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 remains within the required deviation range.

[0042] (3) The optical path adjustment box is used to adjust the optical path difference between the sub-telescopes to the micron level. In the coarse phase detection unit, the two-dimensional dispersion fringe detection technology is used to perform coarse phase detection between the sub-telescopes, and the two-dimensional dispersion fringe analysis technology is used to identify the optical path difference of the sub-telescopes. The optical path difference is adjusted with micron-level precision through the movement of the optical path adjuster on the guide rail. This measurement-adjustment forms a real-time closed-loop measurement and control until the optical path difference is less than λ / 4 (λ is the central wavelength of the coarse phase detection).

[0043] (4) The optical path and pointing consistency adjustment of the sub-telescopes is achieved through the small optical path and tilt adjustment function of the integrated adjuster in the optical path adjustment box. In the phase precision detection unit, the sub-telescopes are subjected to phase precision detection through pupil plane interferometry detection technology, and the optical path difference information of the two sub-telescopes when they reach the position of the zeroing detection unit is obtained in real time. This information is used as input to drive the piezoelectric ceramics inside the integrated adjuster so that the optical path difference is less than λ1 / 20 (λ1 is the central wavelength of the phase precision detection). At the same time, the relative pointing deviation information obtained through the phase precision detection combined with the pointing detection is used to drive the piezoelectric ceramics inside the integrated adjuster to tilt the three mirrors to compensate for the tilt deviation caused by the optical path adjustment, thereby achieving consistency in the 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 of the system does not change due to the change of the optical path. The change of the optical path will cause the exit pupil position of the system to change accordingly, and the distance from the exit pupil position detection will cause the zeroing depth in the zeroing detection to decrease. First, according to the range of optical path change, the piezoelectric ceramics inside the integrated adjuster are driven to roughly adjust the curvature of the three mirrors, and the zeroing detection is performed through the zeroing detection unit. Then, according to the zeroing depth calculated in real time during the zeroing detection, the piezoelectric ceramics inside the integrated adjuster are driven again to fine-tune the curvature of the three mirrors until the zeroing depth change tends to be stable, which means that the exit pupil position adjustment is completed.

[0045] Example:

[0046] The specific steps are as follows:

[0047] (1) Adjust the position and attitude of the sub-telescopes and the beam-combining telescope. The positions of the sub-telescopes and the beam-combining telescope are adjusted according to the detection baseline of the spatially 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 star-planet system to be observed located in the central field of view of each sub-telescope, and the beam-combining telescope and the sub-telescopes maintain the observation configuration.

[0048] (2) Adjust the pointing adjustment mirror of the beam combining telescope so that the beam combining telescope can receive the observation beam from the sub-telescope. Analyze the relative pointing deviation of each sub-telescope through the pointing detection data and phase detection data, rotate the pointing adjustment mirror to ensure that the relative pointing of the sub-telescope remains within the required deviation range, and define this state as the initial state, such as Figure 4 As shown in (a), the system exit pupil position is -25274.35 at this time, and the coordinates of the exit light position are shown in the figure.

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

[0050] (4) When adjusting the optical path, the optical path adjustment box tilts, and the tilt angle is 0.02 degrees around the x-axis. Figure 4 As shown in (c), the exit pupil position becomes -25077.03, and the exit beam is translated. As shown in the figure, the Y coordinate is translated to -1.199906004E+02.

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

[0052] (6) Adjust the deflection angle of the three mirrors and rotate them around the Y axis by -0.000765 degrees, as shown in Figure 4 As shown in (e), the Y-direction offset of the outgoing light beam is adjusted back to the initial state, and the exit pupil position remains unchanged.

[0053] At this point, the optical path adjustment box completes the optical path adjustment while maintaining the original exit pupil position, and the light beam does not shift.

[0054] The contents not described in detail in the specification of the present invention belong to the prior art known to the professional and technical personnel in this field.

Claims

1. A pupil-adaptive optical path adjustment method, characterized in that include: The two optical path adjustment boxes are respectively inserted into the optical paths of the corresponding sub-telescopes of the beam combining telescope in the spatially distributed optical synthetic aperture detection system; The optical path adjustment box is provided with optical elements and a comprehensive adjuster; Adjust the positions of the sub-telescopes and beam-combining telescopes according to the detection baseline requirements of the spatially distributed optical synthetic aperture detection system, so that the stars in the star-planet system to be observed are located in the central field of view of each sub-telescope, and maintain the observation configuration after the adjustment is completed; Adjust the pointing adjustment mirror of the beam combining telescope so that the beam combining telescope can receive the observation beam from the sub-telescope; adjust the relative pointing of the two sub-telescopes so that the relative pointing of the two sub-telescopes remains within the required deviation range; Move the optical path adjustment box to adjust the optical path difference between the sub-telescopes to the micron level; Use the integrated adjuster in the optical path adjustment box to adjust the small optical path and tilt to make the optical path and pointing direction of the sub-telescopes consistent; The curvature of the integrated adjuster in the optical path adjustment box is adjusted to adjust the exit pupil position of the spatially distributed optical synthetic aperture detection system so that the exit pupil position of the system does not change due to the change of the optical path, thereby completing the pupil plane adaptive optical path adjustment.

2. The pupil-adaptive optical path adjustment method according to claim 1, characterized in that: Two through holes are set on one end face of the optical path adjustment box, which are used for light entry and light exit respectively. The end face is defined as the light entry and light exit face. Optical elements and integrated adjusters are set in the optical path adjustment box. Specifically: The three optical elements include: a primary mirror, a secondary mirror, and a tertiary mirror; the optical axes of the three optical elements are parallel to the light entrance and exit surfaces of the optical path adjustment box and are placed in the optical path adjustment box, and the optical centers are on the same straight line; the primary mirror is a parabolic mirror, located between the secondary mirror and the tertiary mirror; the secondary mirror is a hyperbolic mirror, located on the inner wall between the light entrance hole and the light exit hole; the tertiary mirror is a curvature adjustable mirror, integrated with the integrated adjuster, and located at the focus of the secondary mirror; 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.

3. The pupil-adaptive optical path adjustment method according to claim 1, characterized in that: The outgoing light of the sub-telescope enters the beam combining telescope, which includes a pointing adjustment mirror, a beam compressor, an optical path adjustment box, a pointing detection unit, a zeroing detection unit, a phase coarse detection unit, and a phase fine detection unit; specifically: The optical path of each telescope is adjusted in direction by the pointing adjustment mirror of the beam combining telescope 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 divided into three beams, one of which is subjected to pointing detection in the pointing detection unit, one is converged after being dispersed with the light beam corresponding to the other telescope in the coarse phase detection unit for coarse phase detection, and the last beam is also coaxially combined with the light beam corresponding to the other telescope, and then divided into two beams, one of which is subjected to fine phase detection in the fine phase detection unit, and the other is subjected to zeroing detection in the zeroing detection unit.

4. The pupil-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 center of mass detection, analyze the relative pointing deviation of each sub-telescope from it, and rotate the pointing adjustment mirror of the beam combining telescope according to the relative pointing deviation; repeat the above process until the relative pointing of the sub-telescopes remains within the required deviation range.

5. The pupil-adaptive optical path adjustment method according to claim 2, characterized in that: When moving the optical path adjustment box to adjust the optical path length: In the coarse phase detection unit, coarse phase detection is carried out between the sub-telescopes through two-dimensional dispersion fringe detection technology, and the optical path difference of the sub-telescopes is identified using two-dimensional dispersion fringe analysis technology. The optical path difference information is used as input, and 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-telescope is less than λ / 4, where λ is the central wavelength of the coarse phase detection.

6. The pupil-adaptive optical path adjustment method according to claim 2, characterized in that: When the integrated adjuster in the optical path adjustment box is used to adjust the small optical path and tilt: In the phase precision detection unit, the pupil interferometry detection technology is used to carry out phase precision detection between the sub-telescopes, and the optical path difference information when the light of the two sub-telescopes reaches the nulling detection unit of the beam combining telescope is obtained in real time. The 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 central wavelength of the phase precision detection. At the same time, the relative pointing deviation of the sub-telescope drives the piezoelectric ceramic tilt three mirrors inside the integrated adjuster to compensate for the tilt deviation caused by the optical path adjustment, so that the optical path and pointing direction between the sub-telescopes are consistent.

7. The pupil-adaptive optical path adjustment method according to claim 2, characterized in that: When adjusting the curvature of the integrated adjuster in the optical path adjustment box: First, according to the range of optical path change, the piezoelectric ceramics inside the integrated adjuster are driven to coarsely adjust the curvature of the three mirrors, and zero detection is performed through the zero detection unit. According to the zero depth calculated in real time during the zero detection, the piezoelectric ceramics inside the integrated adjuster are driven again to fine-tune the curvature of the three mirrors. The above process is repeated until the zero depth change tends to be stable and the exit pupil position adjustment is completed.

8. The pupil-adaptive optical path adjustment method according to claim 4, characterized in that: The relative pointing deviation of the sub-telescopes is required to be ±0.01″.

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