165 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 atmospheric optical measuring instruments, in particular to an atmospheric coherent length measuring device and a measuring method thereof, and the measuring device comprises a telescope, a focalizer, a primary mirror camera, a star guide mirror, a star guide camera, a PoE power supply communication module, a laser and a computer; the primary mirror camera is connected with the telescope through the focalizer; the focalizer is used for adjusting the focal length of the telescope; the star guide mirror, the PoE power supply communication module and the laser are arranged on the telescope; the star guide camera is connected with the star guide mirror; and the primary mirror camera, the guide star camera, the laser and the computer are all connected with the PoE power supply communication module. The method has the advantages that by adding the focalizer, better and faster focusing work is realized, the telescope obtains clearer fixed star light spot images, and atmospheric coherence length parameters can be calculated more accurately.

The invention discloses a self-co-phase detection method for a plane diffraction spliced telescope with built-in vortex light, and belongs to the technical field of optical imaging telescopes. According to the method, an internal light source of the system is used as beacon light, so that a light beam passes through an optical system in a reverse imaging direction and is emitted in a parallel light form, and then enters the optical system again after being reflected by the front surface of a primary mirror to form a detection light beam carrying co-phase error information; and then, the detection light beam and a vortex light beam in the system generate interference on an image plane, and by acquiring and processing interference fringes in real time and extracting attitude information of the primary mirror under the combined action of forward and reverse errors, decoupling and correction of the piston and tilt errors of the spliced mirror surface can be realized, so that the error correction precision and the overall performance of the system are remarkably improved. In addition, two detectors are arranged in the system, interference fringe detection and system imaging can be achieved at the same time, a beacon light source is taken from the interior of the system, and the defect that a traditional method highly depends on external beacon light is overcome.

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.

An optical system includes an imager, a reflective polarizer, a primary mirror, and a glare trap. The optical system is configured to display a virtual image of an image emitted by the imager after the emitted image is reflected by the primary mirror and transmitted by the reflective polarizer and exits the system through the glare trap. For every light ray emitted by the imager and which exits the system through the glare trap along a first direction, when a light ray is incident on the glare trap along a second direction coincident with and opposite to the first direction, the glare trap transmits at least some of the incident light ray, such that if the transmitted incident light ray attempts to exit the optical system through the glare trap, the glare trap traps the transmitted incident light, transmitting no more than about 2% of the transmitted incident light ray.

A telescope including an optical alignment system. The telescope has a segmented primary mirror and the mirror segments have facets that are used to direct metrology light for aligning the telescope.

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 an active detection method for co-phase errors of a phase shift modulation planar diffraction spliced telescope, and belongs to the technical field of optical imaging telescopes. According to the method, a laser emits a beacon light source at the focal point of a spliced telescope and reversely irradiates a primary mirror of the telescope, a beacon light beam passes through the rear surface of the primary mirror, is reflected by a front surface, then passes through the rear surface and returns along an imaging light path, and a phase shift modulator applies a specific delay phase to a reference aperture. Point spread functions under different modulations are collected through a camera so as to solve co-phase errors of the system, and co-phase error correction is carried out through a phase shift modulator. According to the method, the semi-transparent and semi-reflecting mirror is used for dividing an imaging light path into two parts, the laser is arranged at the other focus, the original telescope imaging light path does not need to be damaged, an external light source does not need to be additionally introduced, and the practicability of the system is improved.

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.

A system for measuring a target gas via laser absorption spectroscopy in an open-air configuration, comprising a mid-infrared distributed feedback interband cascade laser (mid-IR DFB-ICL) having a wavelength selected to correspond with a spectral absorption line of the target gas and first electronic circuitry to control the laser temperature, current and modulation frequency. The mid-IR DFB-ICL is mounted to a heat sink. The system includes an optical component that projects a beam of the mid-IR DFB-ICL onto a distal backscattering directionally-reflective target and an optical receiver assembly that receives a fraction of the laser light that is backscattered from the directionally-reflective target and focuses the collected light onto an uncooled photodetector having a spectral bandwidth and optical configuration selected to optimize signal-to-noise response to received laser light. The optical receiver assembly comprises a primary mirror for receiving laser light backscattered from the directionally-reflective target and focusing the collected light onto the uncooled photodetector.

A vehicle side mirror with hidden blind spot mirror device is provided. The device is comprised of a main mirror with at least one display screen positioned under the top surface of the main mirror. The device provides an improved vehicle side mirror with a blind spot mirror display that is only visible (i.e., illuminated) when a secondary vehicle is detected in the blind spot of the vehicle the device is attached to.

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 primary mirror taper sleeve bonding optical axis positioning device and a positioning method, and belongs to the technical field of optical precision instrument installation and adjustment. A plane is processed at the edge part of a reflecting surface of a primary mirror, so that the plane is parallel to an optical axis processing reference plane; bosses are arranged on the upper end face and the lower end face of a positioning tool respectively, the boss on the lower end face makes contact with a marble table face, and the boss on the upper end face is connected with a primary mirror triangular backboard tool. Through the parallelism of an upper end face boss and a lower end face boss, a primary mirror optical axis machining datum plane is transmitted to a primary mirror triangular backboard tool connecting face, so that the primary mirror optical axis machining datum plane is transmitted to a primary mirror three-point flexible joint end face, and the primary mirror triangular backboard tool is fixedly connected with a flexible joint taper sleeve assembly through the bosses arranged on the primary mirror triangular backboard tool. And three-point flexible joint coplanarity is realized. Meanwhile, the end face of the flexible joint is parallel to a primary mirror machining datum plane, perpendicularity of the primary mirror optical axis and the backboard end face is controlled, and datum transmission of the optical axis is achieved. The method is suitable for positioning the bonding optical axis of the primary mirror taper sleeve of the telescopic system.

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.

The invention relates to the field of spacecraft attitude control, in particular to a load optical axis pointing control system and method for a truss type flexible spacecraft, and the system comprises a truss type flexible spacecraft structure platform, an attitude control module and a load optical axis pointing control module. The attitude control module is used for central star attitude angle fine adjustment and preliminary adjustment of optical load primary mirror optical axis direction. The load optical axis direction control module is used for optical axis direction fine adjustment and micro-vibration suppression. Two independent closed loops of central star attitude angle closed-loop control and load optical axis pointing closed-loop control are constructed, input signal sources, control objects and execution mechanisms of the two control loops are completely decoupled, and the problem of control effect divergence caused by mutual interference in traditional coupling control is solved in principle.

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.

The present invention relates to a hub type automatic focusing lens, comprising a main mirror seat, an upper cover, a hub assembly, a motor assembly, a field of view positioning assembly and a limit switch, wherein the hub assembly and the motor assembly are both arranged in the main mirror seat, the upper cover is fixedly connected to one side of the main mirror seat, the limit switch is fixedly connected to the inner side of the upper cover, the motor assembly drives the hub assembly to rotate to 0° or 90°, the hub assembly is also provided with a trigger device for colliding and triggering the limit switch to stop the motor assembly, and the field of view positioning assembly is arranged on one side of the main mirror seat and is used to lock the hub assembly when it rotates to 0° or 90°. Beneficial effects: fast focusing speed and good optical axis consistency. The manufacturing and installation process requirements are relatively low, meeting the requirements of mass production. The azimuth direction is changed only by interactive transformation between the two positions of 0° and 90°, and the switching speed is extremely fast, meeting the requirements of fastness and maneuverability.

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 invention discloses a rapid assembling and adjusting device for a space beam combining reflector group. The rapid assembling and adjusting device comprises a helium-neon laser (1), a total reflection mirror (2) with a center hole, a rotary table simulation mechanism (3), a reflector diaphragm (4), an autocollimator (5), an internal diaphragm (6), a beam combining box (7) and a primary mirror (8). A helium-neon laser (1), a total reflection mirror (2) with a center hole and an internal diaphragm (6) are coaxially installed on the rotary table simulation mechanism (3) from top to bottom. The rotary table simulation mechanism (3) is arranged at the center of the top surface of the beam combining box (7); the primary mirror (8) is arranged in the beam combining box (7) and is positioned right below the internal diaphragm (6); the mirror surface of the primary mirror (8) is provided with a reflector diaphragm (4); and the autocollimator (5) is erected outside the beam combining box (7), and the emergent light of the autocollimator (5) is consistent with the reflected light path of the primary mirror (8). According to the invention, the autocollimator is adopted to replace laser of different wavebands, is not limited by the adjustment of the target wavebands, is suitable for the adjustment of the combined space beam combining system, and is wide in application range and high in practicability.

The invention discloses a light and small type large-view-field imaging lens, and belongs to the technical field of optical imaging, the light and small type large-view-field imaging lens is characterized in that a primary mirror, a relay reflector and a field lens group are sequentially arranged from an object space to an image space along an optical axis, light emitted by an object space target enters the primary mirror, and after chromatic aberration and aberration are preliminarily corrected through the primary mirror, the light enters the relay reflector; the light is converged by the relay reflector, changes the propagation direction and then enters the central area of the rear surface of the primary mirror, the plane reflection characteristic of the central area of the rear surface of the primary mirror is utilized to enable the light to be turned and enter the field lens group, and the light is focused to an image surface after off-axis aberration is corrected by the field lens group; the primary mirror is a multifunctional plano-convex lens, the front surface of the primary mirror is a traditional refraction convex surface, the rear surface of the primary mirror is divided into an inner area and an outer area, the inner ring area is a standard plane reflecting surface, and the outer ring area is a micro-nano structural surface. The light and small large-view-field imaging lens only comprises at least three elements, and is compact in structure, small in size envelope and convenient to install and use on a motion platform.

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.

The present invention discloses a self-phase detection method for a plane diffraction splicing telescope with built-in vortex light, which belongs to the technical field of optical imaging telescopes. The method uses the internal light source of the system as a beacon light, so that the light beam first passes through the optical system in the opposite direction of imaging and is emitted in the form of parallel light, and then re-enters the optical system after being reflected by the front surface of the main mirror, forming a detection light beam carrying the common phase error information; then, the detection light beam and the vortex light beam in the system interfere with each other on the image plane, and the attitude information of the main mirror is extracted under the joint action of the positive and negative errors by acquiring and processing the interference fringes in real time, so as to realize the decoupling and correction of the piston and tilt error of the splicing mirror, thereby significantly improving the accuracy of error correction and the overall performance of the system. In addition, the configuration of two detectors in the system can realize interference fringe detection and system imaging at the same time, and the beacon light source is taken from the inside of the system, which overcomes the high dependence of the traditional method on external beacon light.

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.