CN108957726B - Quick adjusting method for axisymmetric telescope by taking image plane as reference - Google Patents

Abstract

Translated fromChinese

本发明一种以像平面为基准的望远镜快速装调的方法，装调方法的主要步骤有：（1）用一束出射光束建立一个垂直于像平面且通过其中心的视轴基准；（2）利用次镜顶点法向量与光轴重合的特点对次镜进行装调；（3）在望远镜主次镜之间拉一个十字丝，利用轴对称光学系统旋转对称的特点对主镜进行装调。用于装调的工具具有以下特点：（1）用一个激光器产生一束出射光束作为参考光；（2）出射光束可以进行高精度回转；（3）出射光束可以绕回转轴上的一点进行高精度倾斜调整，且出射光束所在轴线经过其倾斜调整中心。本发明适用于轴对称望远镜的快速装调工作，也可以用于透射式光学模组的安装，装调工具使用简单方便。

The present invention is a method for quickly aligning a telescope with an image plane as a reference. The main steps of the aligning method are: (1) establishing a boresight reference perpendicular to the image plane and passing through its center with an outgoing beam; (2) ) Use the feature that the vertex normal vector of the secondary mirror coincides with the optical axis to align the secondary mirror; (3) Pull a cross between the primary and secondary mirrors of the telescope, and use the rotational symmetry of the axisymmetric optical system to align the primary mirror . The tool used for adjustment has the following characteristics: (1) A laser is used to generate an outgoing beam as a reference beam; (2) The outgoing beam can be rotated with high precision; (3) The outgoing beam can be rotated around a point on the axis of rotation. Precision tilt adjustment, and the axis of the outgoing beam passes through its tilt adjustment center. The invention is suitable for the quick installation and adjustment of axisymmetric telescopes, and can also be used for installation of transmission optical modules, and the installation and adjustment tools are simple and convenient to use.

Description

Quick adjusting method for axisymmetric telescope by taking image plane as reference

Technical Field

The invention belongs to the technical field of optical telescope detection assembly, and relates to an optical telescope assembling technical method, in particular to a method for quickly completing low-precision optical assembling work in a telescope by using a certain tool and method.

Background

At present, in the technical field of detection and assembly of optical telescopes, an optical telescope assembling and adjusting method is that after one telescope is designed and processed, the telescope can normally work only after being assembled and adjusted according to a certain assembling and adjusting technical method. The main task of telescope adjustment is to ensure that each optical component is in the spatial position required by the design. The conventional installation and adjustment method needs a micrometer collimating telescope, a pentaprism, a micro-motion adjusting platform and the like and a large number of tools. The installation and adjustment workload is large, and more workers are needed. In addition, various detuning quantities are generated inevitably in daily operation and maintenance of the telescope, and the imaging quality is reduced due to the various detuning quantities of the telescope, the signal-to-noise ratio is reduced, the target details are lost and the like, so that the detuned telescope needs to be adjusted again in time. For field stations, especially observation stations in Xinjiang, Tibet and the like, the adjustment is difficult and time-consuming. And the field station faces the dilemma of lack of instruments, difficult tooling processing and the like, and the installation and adjustment precision is difficult to guarantee due to the severe environmental factors.

Although the conventional adjustment technology of the telescope is mature, each optical equipment production and research unit has respective perfect adjustment technology and tools. However, specific tooling, fields and process flows are required.

Among them, intensive studies have been made in the detection and evaluation of the amount of imbalance domestically and abroad. A common auto-collimation detection assembly method (research on structural design and adjustment method of a high-altitude element and sub-aperture splicing imaging system [ D ], Changchun university of Catharan science, 2012, 53-58) needs a high-precision plane mirror, a matched reference light source and a detector, has high detection assembly precision, but is sensitive to environmental factors, and has high precision of required tools and high requirements on working environment. The method for detecting and assembling by using tools such as a micrometric collimating telescope, a high-precision auxiliary tool and the like (adjustment and detection of an Ledebe astronomical optical telescope [ J ] optical technology, 1998, 24(3): 27-31) has high detection and assembly precision, but has large workload, various required tools and needs a large amount of personnel for cooperation.

Disclosure of Invention

In order to solve the above problems, the present invention provides a method for quickly assembling and adjusting an axisymmetric telescope based on an image plane, which utilizes the characteristics of an axisymmetric optical system, is based on the basic principle of geometric optics, uses a simple tool, and takes the image plane as a reference, and can quickly and intuitively complete the detection and assembly work.

The technical solution of the invention is as follows: a method for quickly assembling and adjusting an axisymmetric telescope by taking an image plane as a reference specifically comprises the following steps:

the first step, the inclination of the emergent beam is adjusted to make the emergent beam coincide with the rotating shaft of the high-precision rotating mechanism. The error of the included angle between the emergent light beam and the rotating shaft of the adjusting mechanism can be eliminated through the operation of the step.

And secondly, establishing a visual axis reference which is perpendicular to the image plane and passes through the center of the image plane by taking the telescopic mirror image plane to be adjusted as the reference. This step of operation can be accomplished by precise mating of the adjustment tool and the telescopic mirror plane mounting mechanism. As the superposition of the high-precision rotation mechanism of the adjusting tool and the emergent light beam is completed in the previous step, the step only needs to realize that the telescopic mirror plane mounting mechanism is coaxial with the shaft hole of the adjusting tool.

And thirdly, the secondary telescope mirror to be adjusted is adjusted in a translation mode, and the secondary telescope mirror is adjusted to incline or translate so that the fine parallel light beams can be incident on the vertex of the secondary telescope mirror. Since the telescopic instrument terminal is mounted on the terminal support structure and the axis perpendicular to the image plane and passing through its center has been identified in the previous step with the outgoing beam of the alignment tool and used as a visual axis reference, the secondary mirror vertex is here located on the visual axis reference by adjusting the tilt or translation of the secondary mirror throughout the instrument terminal support structure. Thereby realizing the translational adjustment of the secondary mirror.

And fourthly, adjusting the inclination of a secondary mirror of the telescope to be adjusted, adjusting the inclination of the secondary mirror to return the emergent beam incident on the vertex of the secondary mirror to the original path, wherein the included angle between the returned beam and the emergent beam is less than 1'. The step is mainly used for adjusting the error of an included angle between the optical axis of the secondary mirror and the reference of the visual axis, so that the inclination adjustment of the optical axis of the secondary mirror is realized. And enabling the optical axis of the secondary mirror to coincide with the visual axis reference.

And fifthly, the primary mirror of the telescope to be adjusted is adjusted in a translation mode, the space distance between the optical axis of the primary mirror and the reference of the visual axis is observed, and if the distance is too large, the space distance needs to be reduced by adjusting the instrument terminal supporting structure. This step requires evaluation of the spatial distance between the primary mirror optical axis and the boresight reference, which can be reduced by adjusting the instrument terminal support structure if the distance is too large. The threshold value of the spatial distance needs to be calculated from the actual optical system. But usually, when the telescope structure is designed, the space distance is ensured to meet the technical index requirement through machinery. No adjustment is generally required.

And sixthly, preparing for adjusting the inclination of the primary telescope to be assembled, drawing a cross wire with the center positioned on the reference shaft between the primary telescope and the secondary telescope by using a thin wire, rotating the high-precision rotating mechanism of the assembling and adjusting tool and adjusting the inclination of the emergent beam to enable the emergent beam to firstly enter the thin wire and then enter the secondary telescope. The method mainly comprises the steps of marking a point of a visual axis reference by using a cross wire with the center positioned on the visual axis reference, generating a light beam with a certain included angle with the visual axis reference by adjusting the inclination of an emergent light beam, enabling the light beam to be incident on the mirror surface of a primary mirror, and detecting the inclination of the primary mirror by utilizing the rotation characteristic.

And seventhly, adjusting the inclination of the main mirror of the telescope to be adjusted, observing and recording the relative position of the outgoing light beam and the thin line after the light beam is reflected by the main mirror to be adjusted by using a paper screen in four directions of the thin line. And adjusting the inclination of the main mirror according to the relative position of the outgoing light beam reflected by the main mirror and the thin line, so that the center of the outgoing light beam passes through the cross wire in four directions. The step is to utilize the axial symmetry characteristic of the telescope, when the main mirror is inclined, the incident light in different directions does not have the axial symmetry characteristic after being reflected by the main mirror, and the inclination of the main mirror can be adjusted according to the deviation.

And eighthly, confirming the installation and debugging stability of the system, and after standing for a period of time, if the result of the observation step 8 is changed, starting from the step 1 to perform installation and debugging again. This step is to eliminate the change caused by the stress deformation generated during the assembly process after standing.

And ninthly, finely adjusting the primary mirror of the telescope to be adjusted by using the defocused star point image of the fixed star, pointing the telescope to be adjusted to the fixed star near the zenith, keeping the telescope to be adjusted in a fixed star tracking state, replacing the fixed star with an image detector, defocusing the star image, finely adjusting the primary mirror of the telescope to be adjusted to incline according to the eccentricity of the inner ring and the outer ring of the defocused star point image, moving the defocused star point image to the direction that the eccentricity of the defocused star point image is thicker, and finally making the inner ring and the outer ring concentric.

And step ten, if the result of the step 9 meets the imaging quality requirement, namely the focus image is sharp and clear after the inner ring and the outer ring of the focus star image are concentric, the optical adjustment work can be finished. Otherwise, resetting is carried out from step 1.

In the above steps, when the adjustment is performed, the entire adjustment result is difficult to reach an ideal state due to a mechanical structure, parallax, an operation error and the like, so that the calibration and fine adjustment need to be performed by a fixed star. The precision of the step can preferably reach the imaging quality of diffraction limit through simulation calculation and actual operation. The operation of the step only finely adjusts the inclination of the main mirror, and other structures are not detected and adjusted.

Compared with the prior art, the invention has the following advantages:

1. the invention utilizes the characteristics of an axisymmetric optical system, is based on the basic principle of geometric optics, can achieve higher detection and assembly precision by using a simple tool, and has the characteristics of good visualization, intuition, simplicity and convenience.

2. The invention has strong adaptability, can be suitable for various optical systems, has simple and convenient integral structure and is convenient to carry and transport.

3. The invention is insensitive to environmental factors and is convenient for assembly work under complex field conditions.

Drawings

Fig. 1 is a flow chart of optical setup with reference to an image plane.

Fig. 2 is a schematic diagram of a method for establishing a visual axis reference and adjusting a secondary mirror based on an image plane.

Fig. 3 is a schematic diagram of a method for adjusting the main mirror based on the image plane.

FIG. 4 is a verified out-of-focus star map using the method of the present invention.

Detailed Description

The following describes embodiments of the present invention. The following examples are only for explaining the present invention, the scope of the present invention shall include the full contents of the claims, and the full contents of the claims of the present invention can be realized by those skilled in the art through the following examples.

The invention fully utilizes the characteristics of the high-precision slewing mechanism and the axisymmetric telescope, and has simple process, convenient realization and higher precision.

The optical adjustment tool used in the present invention includes a high precision rotation structure, an observation window, a high precision tilt adjustment mechanism, and a low divergence angle laser, and the specific structure is shown in fig. 1. The adjustment tool is connected to the vicinity of the mounting image plane location by a precision-fit adapter. And adjusting the inclination adjusting mechanism of the adjusting tool by utilizing the rotation characteristic of the high-precision rotating mechanism to enable the jump of the outgoing beam of the laser to be less than 30' when the rotating mechanism rotates. When the jitter of the outgoing beam of the laser is less than 30' when the laser rotates along with the rotary mechanism, the outgoing beam at the moment is taken as a visual axis reference. When the adjustment is carried out, the position and the jumping condition of the return beam can be observed through the observation window.

When the telescope is adjusted, the method and the structure for adjusting the primary mirror and the secondary mirror are determined according to the specific telescope. The adjusting method only provides a detecting and adjusting process, and when the specific adjustment is carried out, the adjustment must be carried out according to the existing adjusting structure and mode of the telescope. This is because the specific mechanical structure of each telescope will be different during design, and the specific moving and adjusting structure and mode of the primary and secondary mirrors, the instrument terminal supporting structure, etc. will be slightly different. The present invention will not be described in detail with respect to moving and adjusting the operating means and methods.

The invention relates to a method for quickly assembling and adjusting an axisymmetric telescope by taking an image plane as a reference, which specifically comprises the following steps:

step 1: optical adjustment preparation work, adjusting the inclination of the emergent beam to make the emergent beam coincide with a rotating shaft of a rotating mechanism;

step 2: establishing a visual axis reference which is perpendicular to the image plane and passes through the center of the image plane by taking the telescopic mirror image plane to be adjusted as a reference;

and step 3: adjusting the secondary telescope mirror to be adjusted to translate, and adjusting the secondary telescope mirror to tilt or translate the terminal support structure of the telescope instrument to enable the fine parallel light beams to be incident on the vertex of the secondary telescope mirror;

and 4, step 4: adjusting the inclination of a secondary mirror of the telescope to be adjusted, and adjusting the inclination of the secondary mirror to return an emergent beam incident on the vertex of the secondary mirror to the original path, wherein the included angle between the returned beam and the emergent beam is less than 1';

and 5: the primary mirror of the telescope to be adjusted is adjusted in a translation mode, and the spatial distance between the optical axis of the primary mirror and the visual axis reference is observed and adjusted;

step 6: drawing a cross wire with the center positioned on a reference shaft between the primary mirror and the secondary mirror of the telescope by using a thin wire, rotating a high-precision rotating mechanism of a mounting and adjusting tool and adjusting the inclination of an emergent beam to enable the emergent beam to firstly enter the thin wire and then enter the secondary mirror;

and 7: and adjusting the inclination of the main mirror of the telescope to be adjusted, observing and recording the relative position of the light beam emitted after the light beam is reflected by the main mirror to be adjusted and the thin wire by using a paper screen in four directions of the thin wire, and adjusting the inclination of the main mirror according to the relative position of the emitted light beam emitted after being reflected by the main mirror and the thin wire to ensure that the center of the emitted light beam passes through the cross wire in four directions, thereby completing the adjustment.

Further, the method comprises a verification step:

and 8: finely adjusting a primary mirror of the telescope to be adjusted by using a fixed star defocusing star point image, pointing the telescope to be adjusted to a fixed star near a zenith, keeping the telescope to be adjusted in a fixed star tracking state, replacing an image detector, defocusing the star image, finely adjusting the primary mirror of the telescope to be adjusted according to the eccentricity of an inner ring and an outer ring of the defocusing star point image, moving the defocusing star point image to the direction that the eccentricity of the defocusing star point image is thicker, and finally making the inner ring and the outer ring concentric;

and step 9: and (4) if the result of the step (8) meets the imaging quality requirement, namely the inner ring and the outer ring of the defocused star point image are concentric, and the focus image is sharp and clear, finishing the optical debugging work, otherwise, starting to debug again from the step (1).

Further, the detailed steps of step 1 are as follows:

1.1, a rotating mechanism is arranged in front of a light source, the rotating mechanism is rotated, a rotating shaft of the rotating mechanism is determined,

1.2: observing the shaking amount of the emergent light beam of the light source; and adjusting the inclination angle of the emergent beam according to the shaking amount of the emergent beam, and when the shaking amount of the emergent beam rotating along with the rotating mechanism is less than 30', confirming that the emergent beam is superposed with the rotating shaft of the rotating mechanism, and carrying out the next step.

Further, the detailed steps of step 2 are: and the rotating mechanism is arranged on a telescope detector mounting interface to be debugged through a precisely matched adapter, so that an emergent beam of the rotating mechanism is perpendicular to an image plane and passes through the center of the image plane, and the emergent beam is the visual axis reference.

Further, the detailed steps of step 5 are: and drawing a cross wire with the center positioned on the reference axis between the primary mirror and the secondary mirror of the telescope to be adjusted by using a thin wire, checking the distance between the center of the primary mirror of the telescope to be adjusted and the emergent light beam of the adjusting tool, wherein if the distance is less than 1mm, the adjustment is not needed, and if the distance is more than 1mm, the integral inclination of the terminal supporting mechanism of the detector needs to be adjusted or the translation of the primary mirror needs to be adjusted.

The invention takes an image plane as a reference to carry out the process of quickly adjusting an axisymmetric telescope as shown in figure 1, and takes a certain RC telescope as an example, and the method comprises the following specific steps:

firstly, rotating a high-precision slewing mechanism of an adjusting tool, and observing the shaking amount of an emergent beam of a laser at a far distance; and adjusting the inclination adjusting mechanism of the adjusting tool according to the shaking condition of the outgoing beam at a distance, so that the shaking amount of the outgoing beam of the laser is less than 30' when the outgoing beam rotates along with the high-precision rotating mechanism.

And secondly, the optical adjusting tool is installed on an RC telescope detector installation interface through an adapter in precise fit, so that the emergent light beam of the adjusting tool is ensured to be vertical to the image plane and pass through the center of the image plane, and the emergent light beam of the adjusting tool is the visual axis reference at the moment.

Thirdly, if the error of the auxiliary mirror deviating from the mechanical axis is less than 1mm, if the whole detector terminal interface has the inclination capability, the whole inclination of the detector terminal supporting structure is adjusted to enable the emergent light beam of the adjusting tool to be incident on the cross wire at the vertex of the auxiliary mirror; otherwise, the secondary mirror is adjusted to translate, so that the cross wire at the top point of the secondary mirror is positioned on the emergent light beam of the adjusting tool. The light beam emitted by the adjustment tool is the visual axis reference, as shown in fig. 2.

And fourthly, under the condition that the center of the cross wire at the top point of the auxiliary lens is always positioned on the emergent light beam of the adjusting tool, the secondary lens is adjusted to incline to return the incident light beam in the original path, and the included angle between the returned light beam and the emergent light beam is less than 1'.

And fifthly, drawing a cross wire with the center positioned on the reference shaft between the primary mirror and the secondary mirror of the telescope by using a thin wire, checking the distance between the center of the primary mirror and the emergent light beam of the adjusting tool, wherein if the distance is less than 1mm, the adjustment is not needed, and if the distance is more than 1mm, the integral inclination of the detector terminal supporting mechanism or the translation of the primary mirror needs to be adjusted.

And sixthly, rotating the high-precision rotating mechanism of the adjusting tool and adjusting the inclination of the emergent light beam to enable the emergent light beam to firstly enter the thin line and then enter the secondary mirror, as shown in figure 3.

And seventhly, observing in four directions of the thin line by using a paper screen, and recording the relative positions of the light beams emitted after being reflected by the main mirror and the thin line.

And step eight, adjusting the inclination of the main mirror according to the relative position of the outgoing light beam reflected by the main mirror and the thin line, so that the outgoing light beam passes through the thin line in four directions.

And ninthly, verifying and finely adjusting by using fixed stars near the zenith, finely adjusting the inclination of the primary mirror according to the eccentricity of the inner ring and the outer ring of the defocused star point image, and moving the target to the thicker direction of the inner ring and the outer ring until the inner ring and the outer ring of the defocused star point image are concentric, as shown in fig. 4. Observing the image of the inner and outer circles of the focus, and keeping the inner and outer circles concentric.

The method can quickly finish the optical adjustment work of a certain RC telescope, so that the imaging quality of the RC telescope meets the technical index requirements.

Claims (4)

Translated fromChinese

1.一种以像平面为基准的轴对称望远镜快速装调方法，其特征在于，该装调方法具体包括以下步骤：1. an axisymmetric telescope fast fitting method with an image plane as a benchmark, is characterized in that, this fitting method specifically comprises the following steps:步骤1：光学装调准备工作，调整出射光束的倾斜，使出射光束与回转机构的回转轴重合；Step 1: Preparation for optical adjustment, adjust the inclination of the outgoing beam so that the outgoing beam coincides with the rotation axis of the rotating mechanism;步骤2：以待装调望远镜像平面为基准建立一个垂直于像平面且通过像平面中心的视轴基准；Step 2: Based on the image plane of the telescope to be installed, establish a boresight datum that is perpendicular to the image plane and passes through the center of the image plane;步骤3：调整待装调望远镜次镜平移，调整望远镜仪器终端支撑结构的倾斜或平移次镜使细平行光束入射到望远镜次镜顶点上；Step 3: Adjust the translation of the secondary mirror of the telescope to be installed and adjusted, and adjust the inclination or translation of the supporting structure of the telescope instrument terminal to make the thin parallel beam incident on the vertex of the secondary mirror of the telescope;步骤4：待装调望远镜次镜倾斜调整，调整次镜倾斜使入射到其顶点上的出射光束原路返回，返回光束与出射光束夹角＜1′；Step 4: Adjust the inclination of the secondary mirror of the telescope to be installed, adjust the inclination of the secondary mirror to make the outgoing beam incident on the vertex return to the original path, and the angle between the return beam and the outgoing beam is less than 1';步骤5：待装调望远镜主镜平移调整，观察主镜光轴和所述视轴基准的空间距离，进行调整；Step 5: Adjust the translation of the primary mirror of the telescope to be installed, observe the spatial distance between the optical axis of the primary mirror and the boresight reference, and make adjustments;步骤6：待装调望远镜主镜倾斜调整准备，在望远镜主次镜之间用细线拉一个中心位于基准轴上的十字丝，旋转装调工具高精度旋转机构并调整出射光束的倾斜，使其先入射到细线上，再入射到次镜上；Step 6: Prepare for the tilt adjustment of the primary mirror of the telescope to be installed and adjusted. Use a thin wire to pull a crosshair centered on the reference axis between the primary and secondary mirrors of the telescope. It is first incident on the thin line, and then incident on the secondary mirror;步骤7：待装调望远镜主镜倾斜调整，在细线的四个方向用纸屏观察并记录下光束经待装调主镜反射后出射的光束与细线的相对位置，依据经主镜反射后出射的出射光束与细线的相对位置调整主镜的倾斜，使出射的光束的中心在四个方向上均通过所述十字丝，即完成装调；Step 7: Adjust the inclination of the main mirror of the telescope to be adjusted, observe and record the relative position of the light beam and the thin line after the light beam is reflected by the main mirror to be adjusted with a paper screen in the four directions of the thin line. Adjust the inclination of the main mirror with respect to the relative position of the outgoing beam and the thin line, so that the center of the outgoing beam passes through the reticle in all four directions, that is, the adjustment is completed;步骤8：用恒星离焦星点像精调待装调望远镜主镜，将待装调望远镜指向天顶附近的恒星，并让其处于恒星跟踪状态，换上图像探测器，并使星像离焦，根据离焦星点像内外环的偏心精调待装调望远镜主镜倾斜，使离焦星点像向离焦星点像偏心较厚的方向移动，最终使内外环同心；Step 8: Use the defocused star point image to fine-tune the main mirror of the telescope to be adjusted, point the telescope to be adjusted to the star near the zenith, and make it in the star tracking state, replace the image detector, and make the star image away Focus, according to the eccentricity of the defocused star image, finely adjust the inclination of the main mirror of the telescope to be installed, so that the defocused star image moves in the direction of thicker eccentricity of the defocused star image, and finally the inner and outer rings are concentric;步骤9：如果步骤8的结果满足成像质量要求，即离焦星点像内外环同心,焦点像锐利清晰，则完成光学装调工作，否则，从步骤1开始重新进行装调。Step 9: If the result of step 8 meets the imaging quality requirements, that is, the inner and outer rings of the defocused star image are concentric, and the focal image is sharp and clear, the optical adjustment is completed; otherwise, the adjustment is performed from step 1 again.2.根据权利要求1所述的装调方法，其特征在于，所述步骤1的详细步骤为：2. method according to claim 1, is characterized in that, the detailed steps of described step 1 are:1.1:先在光源前设置一回转机构，转动回转机构，确定回转机构的回转轴，1.1: First set up a rotary mechanism in front of the light source, rotate the rotary mechanism, and determine the rotary axis of the rotary mechanism.1.2：观察光源的出射光束的晃动量；根据出射光束的晃动量调整出射光束的倾斜角，当出射光束随回转机构转动时晃动量小于30″，则确认出射光束与回转机构的回转轴重合，进行下一步。1.2: Observe the shaking amount of the outgoing beam of the light source; adjust the inclination angle of the outgoing beam according to the amount of shaking of the outgoing beam. When the outgoing beam rotates with the rotating mechanism, the amount of shaking is less than 30", then confirm that the outgoing beam coincides with the rotating axis of the rotating mechanism. Proceed to the next step.3.根据权利要求1所述的装调方法，其特征在于，所述步骤2的详细步骤为：通过精密配合的转接件将回转机构安装在待调试的望远镜探测器安装接口上，使所述回转机构的出射光束垂直于像平面且通过像平面中心，此时出射光束即为视轴基准。3. The assembling and adjusting method according to claim 1, wherein the detailed steps of the step 2 are: installing the slewing mechanism on the installation interface of the telescope detector to be debugged through a precisely matched adapter, so that the The outgoing beam of the rotating mechanism is perpendicular to the image plane and passes through the center of the image plane, and the outgoing beam is the boresight reference at this time.4.根据权利要求1所述的装调方法，其特征在于，所述步骤5的详细步骤为：在待装调望远镜主次镜之间用细线拉一个中心位于基准轴上的十字丝，并检查待装调望远镜主镜中心与装调工具出射光束的距离，如果距离小于1mm，则可不做调整，如果距离大于1mm，则需要调整探测器终端支撑机构的整体倾斜或者调整主镜平移。4. The adjustment method according to claim 1, wherein the detailed steps of the step 5 are: a reticle whose center is located on the reference axis is pulled with a thin wire between the primary and secondary mirrors of the telescope to be adjusted, And check the distance between the center of the main mirror of the telescope to be installed and the outgoing beam of the adjustment tool. If the distance is less than 1mm, no adjustment is required. If the distance is greater than 1mm, it is necessary to adjust the overall tilt of the detector terminal support mechanism or adjust the translation of the main mirror.

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