25 results about "Optical telescope" patented technology

This invention provides an optical system and method for free-space quantum key distribution. The optical telescope employs a transmission-type telescope and a simplified rear optical path terminal, effectively avoiding secondary mirror obstruction and vignetting. The optical telescope system has a smaller axial dimension and is lighter than a Cassette-type reflecting telescope of the same aperture, making it more suitable for large-scale use in short-range free-space quantum communication. It can be carried and deployed by a single person and has all-day quantum key distribution capabilities. Furthermore, the transmitting and receiving telescopes are interchangeable, meaning the system can function as both a transmitter and a receiver, extending quantum communication coverage to areas inaccessible by fiber optics and satellites, and enabling rapid deployment in various emergency and unforeseen circumstances.

A kind of telescope active optical correction system correction accuracy testing device, including laser interferometer, multidimensional adjusting table, wave aberration measurement component and plane mirror, laser interferometer is placed in the outside of optical telescope for emitting test light to the inside of optical telescope, to detect the wave aberration data of multiple fields of view;Multidimensional adjusting table is used to adjust the position, angle of optical element in optical telescope, to simulate the situation that telescope imaging quality drops;Wave aberration measurement component is set at the image plane of telescope for measuring the wave aberration after optical telescope imaging quality drops, and plane mirror is used to reflect test light.The present application relates to a kind of telescope active optical correction system correction accuracy testing method, the displacement amount and rotation angle of optical element when comparing when simulating image quality drop and when correcting judge the correction accuracy of active optical correction system, compare wave aberration before simulating image quality drop and after correction, judge whether the image quality after correction reaches the image quality before simulating image quality drop.

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 discloses a large dynamic range imaging device and method, relates to the technical field of remote sensing imaging, and the device is characterized in that a rotating scanning component moves to a corresponding position according to a rotating instruction, and sends received radiation into an optical telescope component, and then converges to a light splitting component; the light splitting component divides the radiation into visible light and infrared rays, and respectively sends the visible light and the infrared rays into a visible light component and an infrared component; the visible light component focuses received visible light and obtains visible light signal data through multi-channel faint light detection; the infrared component collimates, focuses and multi-channel infrared detects received infrared rays to obtain infrared radiation signal data; a controller amplifies and processes the visible light signal data and the infrared radiation signal data, and obtains a ground object target image through data fusion, then determines corresponding ground object target line-of-sight angle information based on the ground object target image, and then generates a rotating instruction and sends the rotating instruction to the rotating scanning component. The application can obtain a remote sensing image with rich and complete data information under low illumination.

There are provided: a light source to generate a laser beam; an optical modulator to superimpose a communication signal on the laser beam; an OHPA to amplify the laser beam; a collimator including a fiber connector and a collimator lens to convert the laser beam amplified into spatial light, and emit the spatial light; an optical telescope to enlarge a beam width of the spatial light and emit the spatial light to a spatial transmission path; a drive mechanism capable of adjusting a focal length of the collimator lens; and a drive controller to determine a drive amount of the drive mechanism in such a manner that a product of a free space loss calculated from a distance between the spatial optical communication transceiver and a spatial optical communication transceiver and a transmission gain determined by a beam spread angle of the spatial light is constant.

an LEO satellite includes a light projecting element that emits emission light to another LEO satellite, an optical telescope, an optical phased array, a light receiving element that receives incident light from the other LEO satellite, a distance measurement unit that measures a distance to the other LEO satellite based on at least one of the emission light and the incident light, and a control unit. The control unit captures the other LEO satellites by scanning emission light using the optical telescope and receives incident light from the other LEO satellites for the other LEO satellites on the same orbital plane, and captures the other LEO satellites by scanning emission light using the optical phased array and receives incident light from the other LEO satellites for the other LEO satellites on different orbital planes.

The utility model provides a laser telegraph telescope system with image acquisition and display functions, which comprises a laser telegraph assembly, an image acquisition and processing assembly, an industrial lens, an industrial lens focusing mechanism, an image acquisition unit and an image processing and output unit, and the image acquisition and processing assembly is arranged at the rear end of an eyepiece of the laser telegraph assembly. The industrial lens is coaxially arranged at the rear end of the laser electric eyepiece, the industrial lens focusing mechanism is arranged outside the industrial lens and used for adjusting the focal length of the industrial lens, the image acquisition unit is connected to the rear end of the industrial lens and used for acquiring image data output by the industrial lens, and the image processing and output unit is arranged at the rear end of the image acquisition unit and used for outputting the image data. The image processing unit is electrically connected with the image acquisition unit and is used for processing and outputting image data; and the image display unit is electrically connected with the output end of the image processing unit and is used for displaying the image data. According to the utility model, telescope image acquisition and processing are added on the basis of the original laser telegraph, and are displayed through the display, so that operators can observe conveniently.

The application discloses a three-dimensional geomagnetic space information measuring total station, which comprises physical sensors, magnetic flux gate sensors, optical telescopes and a host computer, wherein the physical sensors and the magnetic flux gate sensors are connected with the host computer, the physical sensors comprise magnetic sensor probes, horizontal angle sensors, vertical angle sensors and distance measuring sensors; the host computer is composed of a WINCE system, the magnetic flux gate sensors convert analog signals into digital signals through AD converters, the physical sensors, the magnetic flux gate sensors and a single-chip microcomputer in the host computer communicate through a 6-pin RS-232 interface, and the application can utilize multidisciplinary comprehensive magnetic force sensors and electronic angle measuring total stations to integrate, establish a data calculation relationship model of three-dimensional geomagnetic space magnetic declination, magnetic inclination, magnetic north azimuth and magnetic north direction angle and develop a geomagnetic space information one-station automatic measuring instrument, i.e., a total station, on the basis of a geomagnetic space information measuring principle, considering a geodetic survey geometric element measuring method and an environment.

The present application relates to the technical field of laser communication, in particular to a kind of interstellar laser communication failure guide adjustment remote control system, including optical telescope module, laser transmitter module, control module and fault diagnosis repair module, optical telescope module is connected with control module, laser transmitter module is connected with control module, fault diagnosis repair module is connected with control module;After interstellar communication handshaking fails, laser transmitter module emits N laser beams, optical telescope module receives laser beam and uploads to control module, fault diagnosis repair module automatically detects and diagnoses fault reason, and generates corresponding measures, measure instruction is uploaded to control module, control module is recontrolled and adjusted according to the received instruction to controlled object, the stability and reliability of interstellar laser communication are maximized to guarantee.

1. The name of the design product: the base of space optical telescope. 2. The use of the design product: the base of space optical telescope. 3. The design points of the design product: in shape. 4. The picture or photo that can best show the design points: perspective view.

The present application relates to the field of optical telescope technology, and proposes a kind of spectroscopic popular science telescope, including frame body, field lens ocular lens, cemented ocular lens, display screen and ridge prism are connected from top to bottom on frame body respectively;Half house cemented prism is fixedly connected between one side of ridge prism and frame body, and the inside of frame body is connected with light splitting focusing module, and light splitting focusing module includes relay lens large lens, relay lens middle lens and relay lens small lens;Light splitting focusing module is composed of three relay lenses of relay lens large lens, relay lens middle lens and relay lens small lens, and light splitting focusing module is arranged on original observation light path, and original observation light path is divided into the following two ways: one way is observation light path, directly conducted to field lens ocular lens for user naked eye observation;Another way is imaging acquisition light path.Through the above technical scheme, the problem that the existing telescope exists prism observation and imaging light path coincides, sometimes there will be shielding interference, which will affect the user's judgment.

A weatherized optical observing system includes components that include an optical telescope, a gimbal, and an integrated controller. The optical telescope includes an imaging device configured to capture telescope images. The gimbal is configured to move the optical telescope in at least two axes. The integrated controller configured to wirelessly transmit the telescope images, wirelessly receive instructions, identify local weather data, actuate the gimbal based on the instructions, and control the optical telescope based on at least one of the instructions or the local weather data.

This application relates to the field of optical system design technology, and discloses a design method, device, and electronic device for an optical telescope based on a stitched primary mirror. The method includes: determining the current aspherical surface parameters of aspherical stitched sub-mirrors in different layers of the optical system according to the optical system constraints of the stitched primary mirror; iteratively optimizing the current aspherical surface parameters according to a pre-constructed comprehensive evaluation function; obtaining optimized aspherical surface parameters of the aspherical stitched sub-mirrors in different layers that satisfy the design requirements of the comprehensive evaluation function within the target field of view; and the best-fit sphere corresponding to the optimized aspherical surface parameters; and outputting the optimization results. This invention can reduce the manufacturing difficulty and cost of the stitched sub-mirrors, avoid the introduction of complex aberration correction optical elements, and ensure the versatility, multifunctionality, and scalability of the overall system.

1. Name of the product in this design: LED light strip for a space optical telescope. 2. Purpose of this design: The entire product is used to optically magnify the light reflected from objects placed on a table or the light emitted from an external monitor, forming a distant virtual image, which is then displayed through a window; a portion of this product is used as an LED light strip in a space optical telescope. 3. The key design feature of this product is its shape. 4. The image or photograph that best illustrates the design's key points: a 3D model. 5. Other matters requiring explanation: This design patent seeks to protect the partial design of the product; the part covered by the light pink mask is the part not for which protection is sought; the enlarged view of part A is a partial enlarged view of part A in the bottom view; the enlarged view of part B is a partial enlarged view of part B in the front view.

This invention relates to the field of optical telescope technology and discloses a Cassegrain telescope, including a primary mirror assembly, a secondary mirror assembly, a connecting assembly, a telescope top plate, and a telescope base plate; the primary mirror assembly is located on the side of the telescope base plate, and the secondary mirror assembly is located on the side of the telescope top plate. Both the primary and secondary mirrors are made of microcrystalline glass, resulting in minimal surface deformation under environmental changes and maintaining stable optical performance. The carbon fiber support rod of the connecting assembly is made of carbon fiber, which has a low coefficient of thermal expansion and high length stability, thus preventing deformation of the primary and secondary mirror surfaces and relative position shifts caused by environmental temperature changes. The leveling triangle plate is fixed to the telescope base plate, and the secondary mirror fixing plate is fixed to the telescope top plate using locking screws. The clamps of the carbon fiber rod assembly, once locked, limit the relative distance between the primary and secondary mirrors. This multi-stage fixing structure ensures the overall stability of the telescope structure and effectively prevents position shifts during use.

The invention discloses a target-independent automatic image stacking method and device for an optical sparse aperture imaging system, and belongs to the technical field of optical telescopes, and the method comprises the steps: collecting an initial degraded image; applying the same inclination amount to the inclination controller of each sub-aperture, collecting N modulated images, and sequentially subtracting the initial degraded images from the N modulated images in pairs to obtain N difference images; n low-frequency difference images are obtained, one low-frequency difference image is used as a reference image, the remaining low-frequency difference images are subjected to cross-correlation operation in phase parts, local k-time up-sampling calculation is carried out in a neighborhood range of a cross-correlation power spectrum peak position, and refined cross-correlation power spectrum peak offset is obtained; and outputting the relative sub-pixel level offset of the residual low-frequency difference image, and controlling the relative sub-pixel level offset through a tilt controller of a corresponding sub-aperture to realize automatic image stacking of the N-aperture sparse aperture imaging primary mirror in any scene. According to the invention, the complexity of the optical path of the optical synthetic aperture imaging tilt error correction module is reduced.

The application relates to a shipborne optical telescope image despin angular velocity calculation method, which comprises the following steps: 1. based on the ship body pitch angle, the ship body azimuth angle, the ship body roll angle, the camera mounting platform pitch rotation angle and the camera mounting azimuth rotation angle output by a shipborne inertial navigation device, an attitude matrix of a camera coordinate system relative to a geographic coordinate system is established; 2. the attitude matrix of the camera coordinate system relative to the geographic coordinate system established in step 1 is calculated to obtain an attitude matrix of a lens coordinate system at a current time of the camera relative to a lens coordinate system at a previous sampling time, and the obtained attitude matrix of the lens coordinate system relative to the lens coordinate system at the previous sampling time is used to calculate the rotation angular velocity of the image; and 3. the rotation angular velocity of the image obtained in step 2 is subjected to noise reduction processing to remove the angle measurement noise of the inertial navigation device and the angle measurement noise of the rotating mechanism. The application ensures that the reference coordinate systems of each frame of image in the continuously shot images are consistent.

The present invention relates to an optical telescope device (1), comprising: - a mirror (2) having a first concave reflective outer face (2a) and a first flat inner face (2b) opposite the first outer face (2a), the first outer face (2a) being polished; - a reinforcement structure (3) fixed to the mirror (2), the reinforcement structure (3) having a second flat inner face (3b) and a second free outer face (3a), the second inner face (3b) being in contact with the first inner face (2b) along a fixing plane; the second free outer face (3a) being concave, the mirror (2) and the reinforcement structure (3) being symmetrical with respect to the fixing plane. Figure for the abstract: Fig. 1

The invention discloses an installation and adjustment method for a wide-spectrum wide-width hyperspectral camera system, and the method comprises the steps: building a unified installation and adjustment reference of a high-precision reference prism and a special image plane reference tool, employing a modularized and criterion installation and adjustment process, and sequentially completing the wave aberration optimization installation and adjustment of a main optical telescope and the concentric shaft centering installation and adjustment of a spectrometer. And field separator butt joint, spectrograph butt joint and detector butt joint are completed according to strict quantitative criteria. A scientific installation and adjustment process of reference establishment, module installation and adjustment and assembly butt joint is adopted, a strict quantitative criterion is introduced, and the whole process is driven by objective data, so that the problems of non-uniform reference, difficulty in focal plane positioning, low multi-assembly collaborative installation and adjustment precision and poor efficiency in a traditional method are solved; high-precision, high-efficiency and high-consistency installation and adjustment of the wide-spectrum wide-width hyperspectral camera system are achieved, and powerful technical support is provided for the hyperspectral camera system to stably and efficiently obtain high-quality and high-precision hyperspectral image data.

An optical imaging system includes: a first lens system housed in a body of a mobile communication device, the first lens system having a first optical axis, a first entrance pupil spatially fixed in a reference plane associated with the body, and a first focal length; and an optical telescope providing diffraction-limited imaging in a spectral range of at least 486 nm to at least 656 nm. The optical imaging system is configured to: when the optical telescope is inserted between the first lens system and the entrance pupil (EPE) of the eye's visual system, image the EPE onto the first entrance pupil at a basic unit magnification, and vice versa.

There is provided a telescope for use in an optical terminal system configured for free space optical communication, FSOC, configured to operate in earth orbit, and / or for terrestrial line- of-sight links. The optical terminal system comprises the telescope and an optical bench. The telescope (200) is configured to receive an incident light beam (500) and to focus the light beam to a telescope focal plane (250) as input to the optical bench. The telescope comprising: a primary mirror; a secondary mirror; and a tertiary mirror. At least one mirror comprises a freeform mirror configured to control the distribution of light in the focal plane to provide correction of wavefront aberrations across a field of view of the system. Also provided is an optical terminal system comprising the telescope and an optical bench.

The application discloses a three-view-field compact infrared optical telescope system, and belongs to the technical field of aerial infrared detection and investigation. The system comprises a secondary mirror, a primary mirror, a first eyepiece, a second eyepiece and a third eyepiece, and is composed of a small-view-field optical mode, a middle-view-field optical mode and a large-view-field optical mode. The small-view-field optical mode is composed of the secondary mirror, the primary mirror, the first eyepiece, the second eyepiece and the third eyepiece. The middle-view-field optical mode is composed of a middle-view-field first objective lens, a middle-view-field second objective lens, the primary mirror, the first eyepiece, the second eyepiece and the third eyepiece. The large-view-field optical mode is composed of a large-view-field first objective lens, a large-view-field second objective lens, the primary mirror, the first eyepiece, the second eyepiece and the third eyepiece. The primary mirror, the first eyepiece, the second eyepiece and the third eyepiece are an optical fixed group, and the secondary mirror, the middle-view-field first objective lens, the middle-view-field second objective lens, the large-view-field first objective lens and the large-view-field second objective lens are switching groups. The three-view-field compact infrared optical telescope system can realize switching among the three optical view-field modes by replacing the switching groups. The application takes into account the application requirements of the infrared optical detection field, such as small-view-field tracking, middle-view-field identification and large-view-field scanning, and improves the integration rate of the system.

The invention discloses a full-baseline complex coherence degree parallel measurement method of a Michelson interferometer, which belongs to the technical field of optical telescopes and realizes parallel measurement of full-baseline complex coherence degree by directly decoupling interference fringes of all baselines through a single-frame image surface speckle image. The method comprises the following specific steps: performing frequency domain band-pass filtering on a collected image surface speckle image; the stripe intensity sampling spacing is refined through frequency domain up-sampling; linear projection integration is carried out along the vertical direction of each base line, and integration signal intensity is collected; eliminating irrelevant variables to obtain interference fringe intensity distribution of all baseline pairs; and finally, measuring the complex coherence degree of each group of stripes by using an ABCD method. The complex coherence degree of all the baseline pairs can be synchronously obtained only through digital image processing without additional optical elements, and the method has the advantages of being simple in structure, high in anti-noise capacity, easy and convenient to operate, good in portability and the like, and is suitable for dark and weak observation scenes.

The application discloses a large-field compound eye telescope system suitable for daytime observation, and belongs to the technical field of optical system design. The system comprises a main mirror, a compound eye optical unit, a refractive 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 angle pyramid prism structure to divide the focal plane of the main mirror into x sub-visual fields. The refractive correction mirror group unit comprises n correction mirror groups with built-in visual field diaphragms. The inner wall of the main mirror chamber is provided with a concentric ring light shield plate group. Through optical splicing of the compound eye structure, large-field observation is realized. By using the built-in visual field diaphragm and combining multiple scattering absorption of the light shield plate group, the strong background stray light in daytime is significantly suppressed, and the stray light coefficient of the system is lower than 1.11*10 ‑7 The application solves the technical problem that the existing optical telescope cannot perform high-contrast large-field observation in daytime, and realizes all-weather monitoring of near-earth celestial bodies.