38 results about "Guide star" patented technology

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.

Methods, devices and systems are described that enable improved determination of wavefront errors associated with light traveling through turbulent media, such as through the atmosphere. The described systems use a Rayleigh-Raman polychromatic laser guide star (RRPLGS) to measure the tilt at the wavelength of observation by making use of the dispersion of the refractive index of air and differential tilt measurements at multiple combinations of wavelengths based on the Rayleigh and Raman back-scattered light. The described RRPLGS systems have a number of advantages, including scalability of returned flux and flexibility in selection of short wavelengths, allowing for a combination of multiple tilt measurements, and enabling characterization of the turbulent media without relying on photons from the object of interest.

The present invention discloses a Shack-Hartmann wavefront sensing system and method based on focus scanning. The detection light beam is conjugated with the scanning device through the first 4f system. The light beam after passing through the scanning device passes through the pinhole and the second 4f system, and finally enters the Shack-Hartmann wavefront sensor. During the focus scanning process, the scanning device deflects the light beam so that different positions of the focused light spot pass through the pinhole at the focal plane of the second 4f system respectively, and the light field phase gradient under different spectra is detected by the Shack-Hartmann wavefront sensor; during the reconstruction process, the light field phase gradient under different spectra is summed with the tilt phase compensated by the scanning device to obtain the corresponding real phase gradient. Finally, the real phase gradient under different spectra is synthesized into a complete phase gradient distribution by using the light spot synthesis method, thereby reconstructing a large dynamic range wavefront. The present invention can greatly improve the dynamic range of the Shack-Hartmann wavefront sensor and can effectively detect the wavefront of multiple guide stars.

The invention relates to the technical field of atmospheric optical measurement, in particular to an atmospheric coherence length measuring device and method with a laser indication function, and the device comprises a telescopic module, a star guiding module, a laser star pointing module, a power supply communication module and a control module. The control module controls the laser star pointing module to carry out laser star pointing through the power supply communication module, so that the star pointing function is convenient to carry out; through laser indication of the laser star pointing module, star finding work can be better carried out, and long-time work can be carried out.

The invention discloses a ground-based high-resolution celestial body imaging method based on lucky imaging, relates to the field of astronomical observation, and is technically characterized by aiming at the problems of limited application scene and the like of a lucky imaging method based on preceding-stage adaptive optical correction. By reducing the number of the required pupil planes, the image signal-to-noise ratio of the beacon light is improved, the requirement on the guide star brightness is reduced, and the observable astronomical target range is expanded. Furthermore, an initial value of an iterative algorithm is replaced by a phase solved by a historical frame, so that the convergence speed of the iterative algorithm is improved. According to the iterative algorithm, the residual wavefront with relatively low aberration can be obtained through single-step iteration, so that the time bandwidth is improved while the correction precision of the system is ensured, and meanwhile, the lucky frame proportion of a post-stage lucky imaging system is improved. The method has the advantages that the preceding-stage adaptive optical system has higher correction efficiency, the complexity of an off-pupil image acquisition system is reduced, and compared with a traditional method, the method has excellent image quality improvement capability under various intensity turbulent flow fields, and is suitable for obtaining high-resolution astronomical images under the conditions of limited guide star intensity and strong turbulent flow fields.

The invention belongs to the technical field of astronomical telescope auxiliary devices, and particularly relates to a solar science popularization telescope visual star guiding device, which comprises a fixed seat, one end of the top of the fixed seat is fixedly connected with a light-transmitting screen, and the light-transmitting screen is vertically arranged; the adjustable reference device is movably arranged at the other end of the top of the fixed seat, and the adjustable reference device is adjusted by taking the center of the light-transmitting screen as a benchmark; the clamping device is detachably connected with the fixed seat, and the clamping device and the fixed seat are used for fixing the telescope therebetween; the elastic clamping device is arranged on the clamping device and used for fixing the telescope to the center of the clamping device so that the adjustable reference device can be parallel to the axis of the telescope. The astronomical observation effect can be improved.

A celestial exploration support program is disclosed. The program can execute, on a computing device, a hopping-path providing function that generates and provides to a user a hopping-path image in which hopping information including a hopping direction and an angular distance from a guiding star to a specific celestial object is reflected on a basic star chart image.

The utility model relates to an integrated astronomical camera which comprises a first imaging CMOS, a second imaging CMOS, a filter disc and a reflector, the first imaging CMOS is located behind the filter disc and used for receiving filtered light rays for imaging, and the second imaging CMOS receives unfiltered light rays through the reflector to achieve a star guiding function; meanwhile, a focusing mechanism is arranged to adjust the position of the second imaging CMOS to achieve the confocal purpose, and multiple types of optical filters such as narrow-band filters are integrated to improve the observation performance under the weak light source condition. According to the invention, the effects of optimizing the space utilization efficiency, improving the imaging precision and enhancing the target tracking capability in a weak light environment are achieved.

The invention discloses a wavefront dot matrix image generation method based on a laser guide star, an optical system and a storage medium, and the method comprises the steps: collecting a laser guide star wavefront dot matrix image with photon noise and distortion interference, and recovering the image into an ideal laser guide star wavefront dot matrix image through maximum likelihood estimation; constructing a wavefront dot matrix image generation model based on a U-shaped neural network; the collected laser guide star wavefront dot matrix image with photon noise and distortion interference is used as training input of a wavefront dot matrix image generation model, the corresponding ideal laser guide star wavefront dot matrix image is used as a training label of the wavefront dot matrix image generation model, and the wavefront dot matrix image generation model is trained; and obtaining a laser guide star wavefront dot matrix image with photon noise and distortion interference, inputting the laser guide star wavefront dot matrix image into the trained wavefront dot matrix image generation model, and generating the laser guide star wavefront dot matrix image without photon noise and distortion interference, thereby improving the correction capability of the optical system.

A feeding and discharging mechanism for plane grinding relates to the technical field of grinding machines and comprises a guide star disc driven by a driving assembly to rotate to achieve feeding and discharging actions, a plurality of feeding holes are annularly and evenly formed in the guide star disc at intervals, and products to be ground are conveyed through the feeding holes. Comprising a feeding positioning device arranged on a guiding star disc and located at a product inlet of a grinding machine, a qualification judging device arranged on the guiding star disc and located at a product outlet of the grinding machine, and an abnormal discharging device arranged on the guiding star disc and located at a discharging port of the grinding machine. A feeding robot matched with the feeding positioning device is arranged at a product inlet of the grinding machine, and a discharging robot matched with the qualification judging device is arranged at a product outlet of the grinding machine. And through the feeding robot, the discharging robot and the automatic judgment device, full-automatic operation of the grinding production line is achieved, and the production efficiency is greatly improved.

The invention discloses an on-satellite autonomous random access and service method for a satellite network in earth-moon space. A satellite antenna in a network node periodically scans the earth-moon airspace and broadcasts access information of a satellite in the space; after the user receives the satellite broadcast information, sending user access application information; the satellite network receives user condition access information and transmits application access information to the constellation network random access planning node; judging a service mode and service time of the user according to the user access application information, and generating user and guide star visibility information; the satellite performs service planning according to the user service application information and the visibility information and generates receipt information; the satellite network broadcasts receipt information to the user; and the user receives the satellite receipt and sends receipt confirmation information to perform service access. According to the random access service system constructed by the invention, the constellation is ensured to provide efficient and reliable communication and navigation services through the scheduling of earth-moon satellite network resources according to user requirements.

The utility model provides a double-sensor astronomical camera which comprises a first sensor and a second sensor, the first sensor is used for shooting images, and the second sensor is used for guiding stars. The camera structure comprises a cooling fin and a refrigerator, one side of the refrigerator is in contact with a circuit board of the first sensor through a silica gel pad, the other side of the refrigerator is in contact with the cooling fin, and effective heat dissipation and shock absorption are ensured. The fixing part comprises an upper panel and a side plate, and the fan is fixed on the upper panel through a soft rubber nail, so that vibration during working is reduced. The vertical position of the second sensor is adjusted through the adjusting structure, the adjusting structure comprises a lower sliding block and an upper sliding block, the upper sliding block moves along the inclined plane of the lower sliding block through rotation of the adjusting screw rod, accurate adjustment of the relative position of the second sensor and the first sensor is achieved, and photosensitive components of the two sensors are located on the same focal plane. And the focal length and the imaging effect are optimized.

The invention discloses a multi-region time-sharing exposure control method for a single-chip image sensor and an application of the multi-region time-sharing exposure control method. The control method comprises the following steps of: logically partitioning a pixel array of a single-chip image sensor according to a shooting scene to obtain a plurality of exposure areas; according to the exposure time of different partitions, a pixel row decoder is controlled to expose the area needing to be exposed; after exposure is completed, the column reading circuit is controlled to read out, and exposure images of all the partitions at different moments and different exposure times are obtained. The method is used in the star guiding process. According to the method, multi-region time-sharing exposure of the single image sensor is realized, and meanwhile, the multi-region time-sharing exposure is applied to the astronomical field, so that a guided star image is acquired and a target image is shot on the same image sensor, the error is smaller when the guide star deviation is calculated, and more accurate guide star correction can be completed. The complex process problem of adjusting the guide star sensor and the main sensor to be in the same plane and the guide star calculation error caused by the adjustment error are avoided.

The application discloses a long-base optical interference system and an optical path collimation method, and comprises an interference terminal and two optical path devices; the optical path device comprises a parallel light tube, a reflecting telescope and a guide star system; parallel light generated by the parallel light tube enters the guide star system after the reflecting telescope; the guide star system comprises a light splitting prism, a first mirror, a first lens, a second mirror and a guide star camera; the parallel light entering the guide star system is split into transmitted light and reflected light by the light splitting prism, wherein the reflected light sequentially passes through a folded axis structure composed of the first mirror, the first lens and the second mirror, and enters the guide star camera; the transmitted light split by the light splitting prism of the guide star system of the two optical path devices is respectively a first light beam and a second light beam; the interference terminal focuses the first light beam and the second light beam after beam combination, and then the first light beam and the second light beam propagate to the interference terminal camera. The system can be applied to outdoor observation, and the method is used for optical path collimation of the long-base optical interference system, so that stable optical interference fringes are obtained.

The invention provides imaging equipment. The imaging equipment comprises a shell, a long-focus imaging assembly, a guide star imaging assembly, a wide-angle imaging assembly and an adjusting mechanism, the long-focus imaging assembly is provided with a first image acquisition end, the guide star imaging assembly is provided with a second image acquisition end, and the wide-angle imaging assembly is provided with a third image acquisition end; a mounting space is formed in the shell; the long-focus imaging assembly, the wide-angle imaging assembly and the adjusting mechanism are arranged in the mounting space; the guide star imaging assembly is connected with the long-focus imaging assembly; the driving end of the adjusting mechanism is connected with the shell and is used for driving the shell to rotate in at least two degrees of freedom; the focal length of the first image acquisition end is greater than that of the second image acquisition end and greater than that of the third image acquisition end. According to the imaging equipment, the long-focus imaging assembly, the guide star imaging assembly and the wide-angle imaging assembly are integrated in the same imaging equipment, so that the problem that the existing imaging equipment is difficult to consider long-distance shooting, viewing shooting and better imaging quality at the same time is solved.

The invention provides a control method of imaging equipment, the imaging equipment and a computer program product. The method comprises the following steps: acquiring an initial image of an equipment body in a current pose by a long-focus imaging module or a guide star imaging module; the initial image is analyzed by the long-focus imaging module or the guide star imaging module, and the current pointing coordinate of the equipment body is determined; and determining the target coordinate of the to-be-observed target, and controlling the adjusting mechanism to drive the equipment body to point to the to-be-observed target based on the deviation between the target coordinate and the current pointing coordinate. According to the method, the long-focus imaging module, the guide star imaging module and the wide-angle imaging module are integrated, so that multiple scene requirements can be met by only one imaging device.

The invention discloses a Greenwood frequency measurement system and a method for using the same. The measurement system comprises an optical receiving system, an optical imaging system, an image acquisition and analysis system, a turntable and control system and an auxiliary system, wherein the optical receiving system comprises an apodization mirror and an optical telescope; the optical imaging system comprises a lens group and a filter; the image acquisition and analysis system mainly comprises a high frame rate CCD camera, an image acquisition card and a monitor; the turntable and control system comprises a servo system and a control system; the auxiliary system mainly comprises a guide telescope, an attenuation plate and a power supply; when the system is used, it can select the optimal target star by assigning different weights through real-time all-sky star catalog screening, considering information such as the magnitude value, spectral type and coordinate position of the star catalog; at the same time, the equipment selected by the system has a complete control interface, can realize the automation of Greenwood measurement, and has the characteristics of simple and convenient use, high measurement accuracy and high automation.

The present disclosure is a method for positioning the light tip of an infrared star guide camera of a 1064nm laser ranging system, and relates to the technical field of space debris laser ranging. The method comprises: performing multi-stage preprocessing on the 1064nm laser beam image collected by the infrared star guide camera; extracting the laser beam profile from the preprocessed image; constructing two types of structural feature lines based on the profile extraction result, and determining the intersection of the two types of structural feature lines as the light tip positioning point. The present disclosure effectively solves the positioning problem caused by strong noise and beam dispersion of the infrared star guide camera, has high positioning accuracy and strong stability, is suitable for complex observation scenes of the 1064nm laser ranging system, significantly improves the reliability of laser debris ranging, and provides key technical support for space debris orbit monitoring.

The present application relates to the technical field of photoelectric detection, and provides a kind of ground-based photoelectric telescope full-automatic star calibration method, comprising: in the corresponding star map of current time, construct the star list for calibration;Iterate the star in the star list, based on the currently guided star, whether the deviation of the current azimuth and the real-time position of the current elevation of telescope is within the first threshold with the position of the star guided in current time;When within the first threshold, the centroid position of the currently guided star is acquired by image acquisition system, and the miss distance of the currently guided star is determined based on the centroid position;Telescope control system calculates miss distance variance based on the miss distance, and judges whether the miss distance variance is within the second threshold;When the miss distance variance is within the second threshold, the calibration data of the guided star is saved, and moves to the next star for automatic calibration, until all the stars in the star list are traversed.

Provided in the present disclosure is a dual-sensor astronomical camera, comprising a first sensor and a second sensor, wherein the first sensor is used for capturing an image, and the second sensor is used for star guiding. A camera structure comprises a heat sink and a cooler, wherein one side of the cooler is in contact with a circuit board of the first sensor by means of a silicone pad, and the other side of the cooler is in contact with the heat sink, thereby ensuring effective heat dissipation and vibration damping. A fixing member comprises an upper panel and side panels, wherein a fan is fixed to the upper panel by means of soft rubber pins, thereby reducing vibration during operation. The vertical position of the second sensor is adjusted by means of an adjustment structure, which comprises a lower slider and an upper slider; by means of the rotation of an adjusting screw, the upper slider moves along an inclined surface of the lower slider, thereby achieving precise adjustment of the position of the second sensor relative to the first sensor, enabling photosensitive components of the two sensors to be located on the same focal plane, and optimizing the focal length and imaging effects.

The present invention discloses a method for quickly identifying dim targets of space debris based on daytime guide star images, comprising the following steps: tracking the target according to the predicted value; collecting the target area image and recording it as the image at time T0; adjusting the telescope pointing azimuth angle ΔA and pitch angle ΔE; collecting the target area image and recording it as the image at time T1; comparing the pixels of the image P0 at time T0 and the image P1 at time T1, taking the pixel difference as the image ΔP, searching ΔP, and obtaining the target centroid coordinates; judging the change in the centroid coordinates and determining the target; calculating the target centroid miss amount and adjusting the pointing. The present application can quickly identify dim targets under strong background noise during the day, and after identifying the target, the deviation of the target angle change from the theoretical value can be quickly obtained, which is used for target pointing and distance deviation correction in future daytime space debris laser ranging.

The present invention provides an on-orbit real-time processing device and method for AIS-guided SAR imaging, which can realize AIS-guided satellite-borne SAR payload to perform positive and side-view imaging of the selected target area, thereby realizing high-resolution detailed inspection and imaging monitoring of distant sea ship targets. The present invention receives AIS messages in real time, performs matching analysis on the messages, monitors whether there are targets of interest in the observation area, and guides the SAR payload to work, thereby realizing high-resolution detailed inspection and imaging monitoring of distant sea ship targets; based on the AIS information of time-sensitive ship targets, on-orbit real-time imaging task planning is performed, and by designing and optimizing the processing flow, the on-orbit SAR payload on the satellite is guided to detect and image the selected ship target, meeting the high real-time, high efficiency, and high reliability requirements of on-orbit applications.

The invention belongs to the technical field of free space optical communication and satellite-ground laser communication, and provides a lens cone deformation testing device and method of a satellite-ground laser communication ground receiving system. In order to solve the problems of high outdoor test cost and narrow application range of the satellite-to-ground laser communication ground receiving system, the lens cone deformation test device of the satellite-to-ground laser communication ground receiving system comprises an image acquisition part, a rotating part, a tracking and pointing driving part and a tracking and pointing control part, a telescope is carried on the rotating part and comprises a main lens barrel and a star guide lens; the rotating part is connected with the tracking and pointing driving part, the tracking and pointing driving part is connected with the tracking and pointing control part, and the tracking and pointing control part is further connected with the image acquisition part; and the tracking and pointing control part is used for tracking fixed stars at different angles in a closed-loop manner, calculating the coaxial deviation angle of the main lens cone and the star guide lens at the corresponding pitching angle and taking the coaxial deviation angle as the deformation amount of the corresponding main lens cone, so that the lens cone deformation amount test aiming at different pitching angles in the outdoor environment is realized.

The invention provides an astronomical camera and a shooting tracking method, and relates to the field of image acquisition. The astronomical camera comprises an optical element, a first sensor, a second sensor and a control chip, the first sensor is configured to receive optical information transmitted through the optical element and output target celestial body tracking data; the second sensor is configured to receive the optical information transmitted through the optical element and output target celestial body shooting data; and the control chip is connected with the first sensor and is configured to track and shoot the target celestial body according to the target celestial body shooting data under the condition that the tracking module of the astronomical camera tracks the target celestial body according to the target celestial body tracking data. According to the astronomical camera provided by the invention, based on the design of the optical element, the first sensor, the second sensor and the control chip, the astronomical camera can independently realize star guiding and shooting, so that the tracking and shooting quality of the astronomical camera is improved.

The present invention discloses a method for measuring the seeing of a layered atmosphere based on dual small telescopes, and the steps include: two small telescopes simultaneously point to the same guide star region and keep the optical path conjugate; use a direct imaging sensor to shoot the observation images of the two small telescopes; use the aperture diameter, aperture spacing and each guide star offset of the two telescopes as initial input to obtain the overall seeing; use the variance of the above parameters as initial input to obtain the seeing of each atmospheric height layer, and calculate the ground layer seeing, and then inversely calculate the atmospheric turbulence profile at each height. The two small telescopes used in the present invention have small apertures, small volumes, and light weights, and are easy to carry; a rigid tripod is used to limit the two telescopes, which can effectively avoid the influence of relative vibration errors and guide errors; no wavefront sensor is needed, and many defects such as relatively low resolution, limited dynamic range, and high difficulty in accurate calibration of the Shack-Hartmann wavefront sensor can be effectively eliminated.

Herein is presented a method for the adaptive correction of images comprises the steps: (a) capturing a first image with an image capture device; (b) selecting within the first image at least one candidate point and at least two test points; (c) using an iterative phase retrieval algorithm to calculate for each of the at least one candidate points an initial aberration correction for the entire image as if each of said at least one candidate points were guiding stars; (d) comparing the aberrations of each of the at least two test points in each of the initial aberrations corrections; (e) selecting the one candidate point whose initial aberration correction yields suitably similar aberrations for each of the at least two test points and designating said candidate point as a virtual guiding star; and (f) calculating phase corrections for the initial aberrations according to said virtual guiding star.

The utility model discloses an off-axis star guider, an astronomical telescope star guiding assembly and an astronomical telescope. The off-axis star guider comprises a connecting main body, a focusing device and a light path coupler, the focusing device is fixedly connected with the connecting main body, the light path coupler is movably matched with the connecting main body and the focusing device, the light path coupler is provided with a first connecting structure, and the first connecting structure is used for being detachably connected with a star guide camera. According to the astronomical telescope guide star assembly provided by the embodiment of the utility model, the focusing device is used as a part of the off-axis guide star device, can be used for focusing a guide star camera and can also be used for accurately adjusting the position of the prism or the reflector, and when the focusing device is used for adjusting the position of the prism or the reflector, the focusing effect is good. The off-axis star guider can be operated without being detached from a telescope and other equipment, other extra tools are not needed, the off-axis star guider is convenient to use, and the position of a prism or a reflector can be accurately known.

The invention discloses a guide star data-based rack residual error adaptive pointing correction method and system, which are applied to a telescope with a height axis and an azimuth axis. The method comprises the following steps: establishing and initializing a rack model; guide star data acquisition and mass filtering; the sky grid coverage degree is judged; judging a sample number threshold value and removing abnormal samples; carrying out residual feature construction based on rack item contribution and meteorological features; training a rack residual regression model; performing new and old model effect comparison and online updating; and correcting the pointing error on line. Under the condition that extra calibration overhead is not increased, automatic updating of the pointing model is achieved through daily guide star data, the pointing precision and stability under the complex weather and long-term drift condition are improved, the manual calibration burden is relieved, and the method is suitable for a high-automation telescope long-term operation scene.

The invention discloses an astronomical telescope off-axis star guiding device with a focus reducer. The astronomical telescope off-axis star guiding device comprises a telescope, a reflector, a main detector system, a focus reducing lens group, a star guiding detector and the like. The off-axis large-view-field star guide of the telescope is realized, the star guide system shares the main light path of the telescope, the light collecting capability and the stability are higher than those of an external star guide mirror, and the focus compressor device improves the star guide detection view field and is beneficial to finding a proper reference star. The invention also discloses a method for calculating the offset of the guide star, the guide star transmits an image shot in a certain period of time to a program for processing, and the program calculates the WCS coordinate (world coordinate system) of the image in a star map matching manner, so as to extract right ascension and declination information of an image reference point. And the offset of the central point is obtained through comparison with historical data and is fed back to a telescope motion system for correction, so that long-time high-precision observation of the target celestial body is realized.

This invention discloses a computationally adaptive aberration correction imaging method for deep tissue based on upconversion nanoparticle guide stars. A near-infrared fluorescence imaging system is constructed using rare-earth upconversion nanoparticles as guide stars. Fluorescence distortion images of deep tissue samples are acquired through near-infrared excitation, and imaging aberrations are parameterized based on Zernike polynomials. Aberration coefficients are reconstructed using a deep learning model incorporating physical prior constraints. Digital wavefront compensation is performed based on the reconstructed aberration information to achieve deep tissue aberration correction and obtain high-resolution imaging results. This invention eliminates the need for complex optical hardware such as wavefront sensors or deformable mirrors, and can stably achieve aberration estimation and compensation even in 360 μm deep tissue conditions. Compared with traditional aberration correction methods, the correction effect is improved by more than 30%, enabling rapid image correction and high-precision positioning. It solves the problems of weak guide star signals, low aberration correction efficiency, and high system cost in deep tissue imaging, and is applicable to deep tissue optical imaging in fields such as clinical diagnosis, biological cell observation, and drug development.