99 results about "Primary mirror" patented technology

The invention belongs to the field of astronomical telescopes, and particularly relates to a large-aperture spliced telescope adjusting device and method, and the method comprises the steps: starting a light source module, providing a far-field illumination light beam for a spliced primary mirror, and carrying out the confocal adjustment of each sub-mirror through an adjusting mechanism according to the far-field illumination light beam; the light source switching module is used for providing a near-field illumination light beam for the spliced primary mirror, and the near-field illumination light beam is split into two separated sub light beams by the pyramid mirror after penetrating through a splicing seam of the spliced primary mirror; performing dispersion on all the sub-beams through a dispersion prism, and converging the dispersed sub-beams through an achromatic lens to form dispersion stripes; the phase difference of the dispersion fringes is extracted through the camera, and co-phase adjustment is carried out on the sub-mirrors through the adjusting mechanism according to the phase difference of the dispersion fringes. According to the invention, high-precision and high-flux spectral response calibration and co-phase detection of the large-aperture spliced telescope can be realized, so that reliable technical support is provided for construction and operation of a next-generation giant astronomical telescope.

The invention relates to the technical field of optical precision interference measurement, in particular to a correction method for projection distortion detection of a primary mirror of a dynamic interferometer and a related product, and the method comprises the steps: obtaining a first coordinate and a second coordinate; determining a zero distortion point; obtaining an ideal imaging point set and an actual mapping point set after system projection through ray tracing; fitting to obtain a distortion function representing the distortion of the optical system; performing point-by-point correction on a phase diagram obtained by interference measurement, mapping pixel coordinates of the phase diagram into workpiece coordinates, obtaining interference measurement data corresponding to the actual surface of the primary mirror, and completing distortion correction; according to the method for correcting the surface shape projection distortion during interference measurement of the high-precision primary mirror of the large-aperture dynamic interferometer, the problem that in the process of assembling, repairing and developing the large-aperture Twyman type dynamic interferometer, the projection distortion effect of a detection system causes the loss of an accurate matching relation between a workpiece coordinate system and a detection coordinate system is solved.

The invention discloses a ground large-aperture reflector composite support design method and a ground large-aperture reflector composite support structure. The ground large-aperture reflector composite support design method comprises the following steps: S1, determining the position of an adhesive point annular belt of a center support at a center hole of a lightweight primary mirror; s2, determining the position of a distribution circle supported by six points on the back of the primary mirror; s3, designing the size of a force unloading groove at the central support for releasing thermal stress; s4, designing the size and the installation depth of a universal flexible joint supported by six points, and realizing freedom decoupling; and S5, parametric modeling is carried out on the supporting structure, supporting parameters are optimized through finite element analysis, and it is ensured that the optical surface deformation RMS values of the primary mirror at the optical axis level and the 60-degree elevation angle are both not larger than 15 nm. The problem that in the prior art, when a large-aperture reflector is in the environment of large temperature change and large pose change, the optical surface is deformed due to the action of thermal stress and gravity, and the imaging quality is affected is effectively solved.

The invention discloses a multi-wavelength same-viewing-direction laser radar telescope system, and belongs to the technical field of laser radar detection. The system comprises a paraboloid single primary mirror which focuses a specific wavelength optical signal received by a telescope to a focus through a primary mirror paraboloid; the replaceable small hole is fixedly formed in the focus position of the paraboloid single primary mirror; the collimating lens group is used for collimating the telescope focusing light beam penetrating through the replaceable small hole to form parallel light beams; the n dichroic mirror groups are used for dividing the parallel light beams into reflected parallel light beams and transmitted parallel light beams; and the plurality of focusing lens group assemblies are used for focusing the parallel light beams split by the dichroic mirror to the focal points of the focusing lens group assemblies, and the number of the plurality of focusing lens group assemblies is n + 1. Multi-wavelength receiving in the same direction can be achieved, light background noise is suppressed by the secondary diaphragm, view fields of different wavelengths are controlled respectively, the size is small, the light collecting efficiency is high, and noise is low.

The application relates to a mounting and adjusting method of a device provided with an array optical system, and belongs to the technical field of mounting and adjusting methods of optical system devices, and solves the problem of complex mounting and adjusting process of the existing optical system device. The mounting and adjusting method of the device provided with the array optical system comprises an array optical system and an assembly frame suitable for the array optical system; the mounting and adjusting method of the device provided with the array optical system comprises the following specific steps: S1, fixing the image inverting lens structure member to a supporting flange plate; S2, fixedly connecting one end of a connecting support rod with the supporting flange plate; S3, contact connecting the other end of the connecting support rod with an imaging main mirror structure member; and S4, after the imaging main mirror structure member is finely adjusted and the whole optical system can present a clear image, the mounting and adjusting are completed. The application solves the problem of complex mounting and adjusting process of the existing optical system device.

The invention discloses a large-view-field compound eye telescopic system suitable for daytime observation, and belongs to the technical field of optical system design. The system comprises a primary mirror, a compound eye optical unit, a refraction correction mirror group unit and a photoelectric detector unit which are sequentially arranged along an optical axis. The compound eye optical unit adopts a light splitting reflection cube-corner prism structure, and divides a focal plane of a primary lens into X paths of sub-view fields; the refraction correction lens group unit comprises n correction lens groups with built-in field diaphragms; a concentric annular light barrier group is arranged on the inner wall of the primary mirror chamber. Large-view-field observation is realized through optical splicing of a compound eye structure, strong background stray light in the daytime is remarkably inhibited by utilizing a built-in view field diaphragm and combining multiple scattering absorption of a light barrier group, and the stray light coefficient of the system is lower than 1.11 * 10 <-7 >. The technical problem that an existing optical telescope cannot carry out high-contrast large-view-field observation in the daytime is solved, and all-weather monitoring of near-earth celestial bodies is achieved.

The application discloses a kind of big field of view off-axis three-reflection beam expanding optical system's alignment method, when adjusting off-axis three-reflection beam expanding optical system using existing mode, it is solved that there is the problem of long alignment cycle and low alignment precision, the concave off-axis parabolic characteristics of off-axis primary mirror and off-axis three-mirror are used, and it is self-accurate detection using interferometer and self-accurate mirror;The relative position relationship of off-axis primary mirror and off-axis three-mirror can be determined using its focal point;Only need to adjust a specific optical element when adjusting system each time, without adjusting other optical elements simultaneously, greatly reduce the adjustment uncertainty;As can be seen, the alignment method of the application, the adjustment degree of freedom in the alignment process is reduced by half compared with existing experience method, realizes the controllability of off-axis type beam expanding optical system optical path alignment process, improves the alignment efficiency of optical system optical path.

The invention discloses an optical telescope primary mirror assembly and an anti-backlash close-fitting method thereof. The primary mirror assembly comprises a telescope primary mirror, a primary mirror mounting seat, a central mandrel, a pressing ring and a plurality of copper sheets. The primary mirror mounting seat is coaxially connected with the central mandrel through a screw and a positioning pin; the primary mirror of the telescope is embedded in the primary mirror mounting seat, and the central spindle penetrates through the central through hole of the primary mirror to finish coarse positioning of the primary mirror in the primary mirror mounting seat. A plurality of equal-thickness copper sheets are inserted into a circular gap between the central mandrel and the central through hole of the primary mirror at equal intervals, so that accurate positioning of the primary mirror in the primary mirror mounting seat is completed while the gap is eliminated. And a ball fastener is screwed into the threaded through hole in the side wall of the central mandrel, and the head of the fastener abuts against the corresponding copper sheet to realize interference fit. According to the design method, the assembled primary mirror assembly can be completely stable, the stress in all directions is uniform, the extrusion stress can be well conducted after the gravity posture is changed, and the good surface precision of the primary mirror is maintained.

The application is suitable for the field of reflectors, and discloses a reflector and a reflector design method. The method comprises the following steps: obtaining optical parameters of a main mirror body, a distribution mode of reinforcing ribs, support point positions and sizes of taper sleeves, and calculating interval distances of the reinforcing ribs and cutting edge angles; determining positions of the reinforcing ribs on the back of the main mirror body based on the distribution mode and the interval distances of the reinforcing ribs, and forming support holes that are adapted to the taper sleeves at the support point positions according to the sizes of the taper sleeves to obtain an initial version of the main mirror; performing weight reduction processing and enhancement processing on the initial version of the main mirror based on the cutting edge angles to obtain a lightweight main mirror; designing the taper sleeves according to the sizes of the taper sleeves and determining support positions of the taper sleeves; determining an angle between an upper flexible claw of a flexible joint and a line connecting the flexible joint and a center of the main mirror, an angle between a lower flexible claw of the flexible joint and the line connecting the flexible joint and the center of the main mirror, and a width of a first flexible joint groove of the upper flexible claw through simulation analysis, and the method can improve the surface shape precision and the structural stability of the reflector.

A Cassegrain mirror 10 that can be easily detached from a microscope without requiring optical adjustment comprises: a Cassegrain mirror body 2 having a main mirror 22, a sub-mirror 24, a housing 26 that holds the main mirror 22 and the sub-mirror 24, and a barrel 32 that is provided on the outer side of the housing 26 and forms an optical path to a central hole 28; a slider 4 having a through-hole 42 sized to allow a gap to form when the barrel 32 is fitted therein, and an adjustment screw 46 for adjusting the position of the barrel 32 fitted in the through-hole 42; and a stage 6 configured such that the Cassegrain mirror body 2 can be attached to and detached from the stage 6 together with the slider 4. A through-hole 62 communicating with the through-hole 42 of the slider is formed in the stage 6. Shapes for positioning the slider 4 at a prescribed position with respect to the stage 6 by sliding the slider 4 in a prescribed direction once the slider 4 has been brought into contact with the surface of the stage 6 are respectively formed in the slider 4 and the stage 6.

This invention relates to an array optical system, an apparatus equipped with an array optical system, and an assembly and adjustment method, belonging to the field of optical imaging, and solves the problems of small field of view and large front-end diameter in existing optical systems. An array optical system includes an imaging primary mirror and an image-rotating mirror group; the primary mirror is used to transmit visible light rays to form a primary imaging visible light real image plane, and the image-rotating mirror group is used to transmit visible light rays to form a secondary imaging visible light real image plane. This invention solves the problems of small field of view and large front-end diameter in existing optical systems.

An optical device comprises a plurality of optical components comprising at least one primary mirror and further comprising at least one scanning mirror component and / or at least one spatial light modulator and / or at least one digital mirror, wherein the plurality of optical components are configured to direct light from an input / output module to an objective module and from the objective module to the Input / output module and to manipulate a position and / or pattern of the light; and a mono-block structure In which the plurality of optical components is mounted, wherein the mono-block structure is a continuous single structure having walls and a base.

The utility model relates to the technical field of telescopes, in particular to an all-air air conditioning system for thermal control of a telescope dome. The all-air air conditioning system for thermal control of the telescope dome comprises a shell; the air return assembly is arranged in the shell, the air return assembly is provided with a first air return pipe, and the first air return pipe is communicated with the main mirror chamber; the air supply assembly is arranged in the shell, the air supply assembly is provided with a fresh air pipe and an air supply pipe, the fresh air pipe is communicated with the outside, and the air supply pipe is communicated with the main mirror chamber; the temperature control assembly is arranged in the shell, the temperature control assembly communicates with the fresh air pipe and the air supply pipe, and the temperature control assembly is used for heating or refrigerating air in the air supply pipe; and the detection assembly comprises sensors arranged in the main mirror chamber, the air supply pipe and the outside, and the sensors are connected with the temperature control assembly so as to transmit detected temperature information to the temperature control assembly. The air return assembly, the air supply assembly and the temperature control assembly are integrated in the shell, and the whole air conditioning system is simple in structure and convenient to control.

The application discloses a kind of optical synthetic aperture imaging system sub-aperture baseline accurate measurement methods, the method specifically is: first, two femtosecond laser ranging probes are installed on respective miniature adjusting frame in opposite direction, ensure that optical axis is parallel, opposite direction is regarded as sub-aperture baseline measuring instrument, it is placed in the reference mirror of known interval and carries out two probe interval calibration, then it is respectively moved to each sub-aperture primary mirror and the conical lens installed on system optical axis, the distance of each sub-aperture primary mirror and fixed conical lens is measured respectively, then according to the structure parameters of sub-aperture and conical lens, the entrance pupil baseline is calculated.The method solves the problem that the sub-aperture entrance pupil baseline in the optical synthetic aperture imaging system with variable baseline and invariable baseline is difficult to accurately and simply measure, provides technical support for the measurement and control of imaging system pupil mapping error, and further provides technical support for the observation field of view and observation efficiency of imaging system.

According to the full-plastic large-aperture wide-angle telescope, firstly, an outer rotating cylinder rotates in a cylinder sleeve, so that the upper angle and the lower angle of a main telescope body can be roughly adjusted; then the fine tuning device works to drive the inner rotating column to rotate in the outer rotating cylinder, and the design can realize fine tuning of the observation angle of the telescope; when an observer observes, the direction of the telescope can be accurately adjusted through the fine adjustment device, a target can be clearly presented in a visual field, any fine observation details are not missed, and the observation accuracy is remarkably improved; in addition, due to the arrangement of the locking device, the outer rotating cylinder can be firmly locked on the cylinder sleeve; after an observer adjusts the angle of the telescope, the telescope is fixed through the locking device, so that the telescope can be kept stable in the observation process, angle deviation caused by external interference or mistaken touch is avoided, the stability and continuity of the observation process are ensured, and a powerful guarantee is provided for obtaining a high-quality observation result.

A large-aperture reflective zoom and laser communication integrated camera is disclosed, relating to the fields of optoelectronic imaging and laser communication technology. It addresses the technological gap where liquid zoom lenses cannot be applied to large-aperture RC systems, and the problem of relying on additional components for integrated visible light imaging and laser communication, making it difficult to balance lightweight design and high performance. The camera consists only of a primary mirror, a liquid zoom lens array, a grating film, a visible light detector, and an infrared detector. The front of the liquid zoom lens integrates a multi-layer liquid zoom lens array, with each layer having a different focal length. Independent drive circuits electrically control and adjust each lens layer to eliminate aberrations and adjust the focal length for optical systems of different apertures. The grating film on the back exhibits high reflectivity to visible light and high transmittance to 1550nm laser light, enabling visible light to form an RC structure imaging optical path, while the laser light is transmitted to complete communication. This invention can be widely applied in aerospace, aviation, and ground observation scenarios.

This invention relates to an optical system assembly frame, a device for assembling an optical system, and an assembly and adjustment method, belonging to the field of optical imaging devices, and solves the problem of complex structures in existing optical system devices. The assembly frame includes an imaging primary mirror structure, an image-rotating lens structure, a support flange, and a connecting rod; one end of the connecting rod is fixedly connected to the support flange by a fixing bolt, and the other end of the connecting rod is connected to the imaging primary mirror structure by an adjusting screw; the image-rotating lens structure is screwed to the support flange. This invention achieves a simple structure for the optical system assembly frame.

The application provides a telescope main mirror protection device, which comprises a support frame, a protection cover plate hinged to the support frame on one side of a mirror surface, the protection cover plate comprising a first cover plate and a second cover plate arranged in a folding manner, a driving mechanism connected to the protection cover plate, the driving mechanism being capable of controlling the first cover plate and the second cover plate to rotate, so that the first cover plate and the second cover plate are unfolded to cover the main mirror surface or are folded to expose the main mirror surface, and the first cover plate and the second cover plate are arranged in a folding manner on one side of the mirror surface when the telescope is not used, so that the structure of the protection device is more compact, the volume occupied by the protection device is reduced, and the driving mechanism can drive the protection cover plate to be unfolded or folded, so that the user does not need to manually unfold or fold the large-sized protection cover plate.

The invention provides a rotating arc ultra-light compact space remote sensing concave mirror device aiming at the pain points that an earth observation space telescope is difficult to deploy due to a large aperture, high in cost and inconvenient to transport, an integrated double-fan-shaped paraboloid primary mirror is taken as a core, and two fan-shaped sub-mirrors are symmetrically divided based on a complete paraboloid mirror of 10m or above; a stable-shape, high-temperature-resistant and low-temperature-resistant high-performance ceramic material including ultrahigh-modulus silicon carbide is adopted, water-based colloidal forming is used as a core process, and a'thickness gradient + honeycomb 'lightweight design is matched, so that the weight is reduced by more than 40%, and the surface precision reaches lambda / 50; a mainstream rocket fairing is adapted through vertical storage, a mirror body does not need a folding mechanism, a view field is complemented by means of coaxial rotation, fan-shaped scanning equivalent view field distortion generated by rotation of a double-fan-shaped primary mirror is accurately corrected through a ground AI image restoration system, 0.1 m-level and higher ground resolution and wide-view-field collaborative observation is achieved, and the system is simple in structure and convenient to use. The device has the advantages of being sufficient in rigidity, high in reliability and adaptive to the space environment, and meets the requirements of accurate measurement and wide coverage of earth observation.

The application discloses a high-performance three-mirror compact range antenna measurement system based on NURBS, combines a non-uniform rational B-spline curve surface fitting algorithm with a terahertz three-mirror compact range design, gives a new application of the non-uniform rational B-spline modeling technology according to electromagnetic background and aperture field distribution of a terahertz frequency band, realizes shape conversion of a beam aperture section from a circular shape to a square shape, takes into account the advantages of the B-spline, can realize free distribution of a grid, obtains a shaped surface of a compact range aperture meeting requirements, and solves the adaptation problem of the non-uniform rational B-spline in the shaping surface design process of the three-mirror compact range. In addition, in the process of the three-mirror compact range design, a good energy mapping condition is explored, the energy attenuation relationship function of the edge of a quiet zone is optimized by adjusting light and a propagation path, the energy dispersion problem caused by diffraction of light at the edge of a primary mirror is further solved, and the performance of the whole three-mirror compact range system is improved.

The application discloses a kind of patch mirror translation error correction methods for extended target, belong to optical imaging technical field.The method for realizing of the present application is: for the optical system of the block type primary mirror of having one piece reference mirror and one piece mirror to be adjusted, to any extended target imaging;Establish the relationship between the reciprocal of the power spectral density of image at the secondary peak position of optical transfer function under wideband spectrum illumination and the translation error of mirror to be adjusted, solve the translation error of mirror to be adjusted using the relationship;Adjust the translation of mirror to be adjusted;Repeat the process of calculating the translation error of mirror to be adjusted until the translation of mirror to be adjusted meets the threshold requirement;For the block type primary mirror optical system containing multiple mirrors, adjust the translation of mirror one by one in turn until all mirrors are adjusted, and the translation error correction is complete.The present application has the advantages of large dynamic range, few iteration times and fast convergence speed, and is suitable for on-orbit translation error correction of telescope with block type primary mirror.

The present application relates to a kind of diffraction polarization imaging systems, including two major modules of diffraction imaging system, focal plane detector, wherein the diffraction imaging system includes a diffraction primary mirror and a set of Schupmann achromatic structure.Target radiation light passes through front aperture and diffraction primary mirror, then after diffraction primary mirror Schupmann achromatic lens group is used to correct chromatic aberration of light emitted by diffraction primary mirror, and converging lens is used to converge into the focal plane polarization detector.Light can be detected by focal plane detector to 0 °, 45 °, 90 °, 135 ° polarization image, and polarization degree and polarization angle image can be solved by Stokes vector method.The above-mentioned diffraction polarization imaging system uses a diffraction primary mirror, a set of Schupmann achromatic structure and a focal plane detector, four different angle polarization images are obtained simultaneously by one-time exposure, the number of imaging system lenses is greatly reduced, and the cost and complexity of the system are reduced.

The application discloses a kind of non-spherical optical primary mirror center axis offset angle calculation method, solve the technical problem that imaging quality is reduced due to center axis offset in the process of non-spherical optical primary mirror assembly, a kind of non-spherical optical primary mirror center axis offset angle calculation method is provided, center axis offset can be effectively detected and corrected, improve optical system imaging quality, reduce assembly difficulty, improve production efficiency, its flexibility and adaptability make it perform well in various high-end optical application scenarios, different sizes and shapes of non-spherical optical primary mirror have applicability, whether small or large optical system, applicable to a wide range of optical equipment and instruments.

The invention discloses an electronic following type laser unit which comprises a rotating disc, a transmitting / receiving end, a substrate, a transmitting / receiving control panel, a rack and a driver. The rotating disc is driven by an azimuth driver to rotate by 360 degrees, and a central hole is provided with a connecting device with a shaping unit; the transmitting / receiving end comprises a primary mirror, a reflecting mirror, a pitching driver and a substrate, and the pitching driver drives the primary mirror to deflect. The mm laser emission heads / detectors on the substrate are arranged in a circumferential array, the installation shaft of the concave spherical substrate device faces the center of the sphere, and the plane substrate is provided with the spherical lens. The transmitting / receiving control panel controls the device to be lightened / operated to form a dynamic array rotating around the axis of the shaping unit, the arrangement direction is matched with the deflection angle of the primary mirror, efficient scanning can be realized without mechanically rotating the array, the structure is reliable, and the device is suitable for airspace detection and other scenes.

The utility model discloses a device for synchronously fixing and locking the side surface of a primary mirror of a reflecting telescope. The device comprises a primary mirror holding claw, a synchronous locking ring, a locking screw, a locking device bottom plate, a locking device fixing screw and a primary mirror bottom plate, according to the device, rotation of the synchronous locking ring is converted into axial thrust on the side edge of the primary mirror, the primary mirror holding claw is pushed to gradually press the primary mirror, the contact face and pressure of the primary mirror holding claw and the primary mirror holding claw are increased at the same time, and it is ensured that the side edge of the primary mirror is pressed and fixed in a face contact mode while the primary mirror is pushed to the center of an optical axis. Compared with a traditional primary mirror side face locking mode, the problems of primary mirror eccentricity, complex installation and debugging and the like caused by stress concentration and asynchronous multi-point adjustment of a traditional device are solved.

The present application provides a compact cassette telescope dual-field optical system, belonging to the technical field of optical detection, including a narrow-field telescope system and a wide-field telescope system. The working surfaces of the narrow-field primary mirror and the wide-field primary mirror face the same side, and the working surfaces of the narrow-field primary mirror and the wide-field primary mirror are staggered. The telescope exit pupil positions of the narrow-field telescope system and the wide-field telescope system coincide, and the telescope exit pupil diameters are consistent. When the narrow field of view is working, the narrow-field folding reflector faces the central hole of the narrow-field primary mirror, and the wide-field telescope eyepiece group is located between the narrow-field folding reflector and the wide-field folding reflector. The outgoing light rays of the wide-field telescope eyepiece group are all located on the back of the narrow-field folding reflector; when the wide field of view is working, the narrow-field folding reflector is located outside the outgoing light range of the wide-field telescope eyepiece group. The optical system structure of the present application is compact and avoids the problem of a large wide-field obstruction ratio after the cassette system is zoomed.

The utility model relates to the field of optical sighting telescopes, in particular to a combined optical sighting telescope which comprises a main telescope body, a sub-telescope body, a bottom plate b, a ratchet wheel, a pawl and a guide rail b. A guide rail a is arranged at the bottom end of the main mirror body, and a fixing rod is rotationally arranged on the outer side of the guide rail a. The sub-lens body is arranged at one end of the main lens body, a rotating block is arranged on one side of the sub-lens body, supporting blocks are arranged on the two sides of the rotating block, and a bottom plate a is arranged at the bottom ends of the two supporting blocks; the bottom plate b is arranged on the bottom surface of the bottom plate a; the ratchet wheel is rotatably arranged on the upper end surface of the bottom plate b; the upper end of the ratchet wheel is rotatably arranged on the bottom surface of the bottom plate a; the pawl is arranged on the upper end face of the bottom plate b, and the tip of the pawl is movably clamped to the outer side of the ratchet wheel. The guide rail b is arranged at the bottom of the bottom plate b. A fixing mechanism can be arranged on the side face of the mirror body to fix the mirror body, operation is convenient, and the relative position between the sub-mirror body and the main mirror body can be finely adjusted after installation.

The invention discloses a high-precision surface shape detection supporting device for a large-aperture optical element, which solves the problem that the supporting force of an existing surface shape detection supporting device for an optical primary mirror to the optical primary mirror is difficult to ensure to be equal everywhere, and specifically comprises a supporting base, an azimuth mechanism, a pitching mechanism and a lifting mechanism, the lifting mechanism is arranged on the azimuth mechanism, and the lifting end is connected with a to-be-tested optical element; the azimuth mechanism is rotationally arranged on the supporting base and used for driving the lifting mechanism to rotate in the circumferential direction; and the pitching mechanism is arranged on the supporting base, is rotatably connected with the azimuth mechanism and is used for adjusting the pitching angles of the azimuth mechanism and the lifting mechanism. According to the surface type detection supporting device, azimuth adjustment, pitching adjustment, lifting adjustment and mutual superposition of the azimuth adjustment, the pitching adjustment and the lifting adjustment of the installation plane of the optical element to be detected can be achieved, and flatness adjustment can be better guaranteed.

The utility model belongs to the technical field of night vision devices, and particularly discloses a high-reliability fast-assembly four-eye night vision device main mirror body. Connecting cavities are formed in the two sides of the interior of a main mirror frame of the main mirror body respectively, the image intensifiers are arranged in the connecting cavities in a sliding mode, the two connecting cavities in the main mirror frame are communicated with each other, and clamping grooves are formed in the upper wall and the lower wall of the main mirror frame respectively. Two conductive elastic sheets are respectively fixed on the two side surfaces of the circuit board at intervals up and down and are respectively elastically propped against the positive electrode and the negative electrode of the image intensifier; and the conductive contact pins penetrate through the upper wall of the main mirror frame and are electrically connected with the conductive elastic sheets of the circuit board. According to the utility model, the upper and lower walls between the two connecting cavities in the main mirror frame are respectively provided with the clamping grooves into which the circuit board can be inserted, and the two side surfaces of the circuit board are respectively and vertically fixed with the conductive elastic sheets which elastically abut against the positive and negative electrodes of the image intensifier, so that the image intensifier and the circuit board are convenient to install, and the electrical connection is stable and reliable after the image intensifier is installed; the device has the characteristics of compact structure, convenient installation and reliable connection.