Design of Digital Binoculars Image Stabilizing Optical System

2013 ◽  
Vol 552 ◽  
pp. 85-92
Author(s):  
Chen Hao Ma ◽  
Yue Gang Fu ◽  
Chun Hua Luo ◽  
Dong Hu Zhang ◽  
Yan Liu
Keyword(s):  
Field Of View ◽  
Digital Cameras ◽  
Beam Angle ◽  
Long Distance ◽  
Entrance Pupil ◽  
Image Stabilization ◽  
Rotation Theorem ◽  
Telescope System ◽  
Visual Light ◽  
Entrance Pupil Diameter

Digital binoculars is the combination of digital cameras and telescopes, it not only can observe the details of the long distance target but also can record it. The field of view between photographic field lens and telescope system is the same. This paper designs the telescope system on basis of the theory of dynamic optics. The system works in visual light waveband. The field of view is , the magnification is eight and the entrance pupil diameter is 32mm. prism is selected as the image rotation prism and image stabilization prism. In order to obtain clear images in a dynamic circumstance, we utilize the rotation theorem of prism to analyze the relation between jitter compensated lens and luminous beam angle. We can calculate the position of compensated lens. So it can achieve the jitter compensation. Finally, this paper takes an application as an example. If the jittered angle is , the displacement of pixel is calculated to 1.061mm. The displacement of the compensated lens is 2.84mm. At the same time, the light still arrives to the eyepiece by the original track. So image stabilization is relative to the reference coordinate, as a result we can get the stable image.

scholarly journals Catadioptric Optical System Design of 15-Magnitude Star Sensor with Large Entrance Pupil Diameter

Sensors ◽  
2020 ◽  
Vol 20 (19) ◽  
pp. 5501
Author(s):  
Yang Bai ◽  
Jianlin Li ◽  
Rongwei Zha ◽  
Ying Wang ◽  
Guangzhi Lei
Keyword(s):  
Optical System ◽  
Attitude Control ◽  
Pupil Diameter ◽  
Focal Length ◽  
Field Of View ◽  
Star Sensor ◽  
Spherical Lens ◽  
Entrance Pupil ◽  
Secondary Mirror ◽  
Entrance Pupil Diameter

The optical system is one of the core components for star sensors, whose imaging quality directly influences the performance of star sensors for star detection, thereby determining the attitude control accuracy of spacecrafts. Here, we report a new type of optical system with a catadioptric structure and a large entrance pupil diameter for a 15-magnitude star sensor. It consists of an improved Cassegrain system (R-C system), an aperture correction spherical lens group and a field of view correction spherical lens group. By embedding the secondary mirror of the R-C system into the output surface of the negative spherical lens of the aperture correction spherical lens group, the blocking of incident light is eliminated from the secondary mirror holder. After the structure optimization, the catadioptric optical system (COS) had a spectral range of 450 nm–950 nm, an entrance pupil diameter of 250 mm, a half-diagonal field of view of 1.4° and a focal length of 390 mm. By using theoretical calculations and experimental measurements, it was verified that the COS, with the ability to correct astigmatism, lateral color and distortion, can fulfill the detection of 15-magnitude dark stars.

scholarly journals Optical Design of the Goaly3 Multi-Mirror Telescope System with a Wide Field of View

2021 ◽  
Vol 11 (3) ◽  
pp. 1200
Author(s):  
Junliu Fan ◽  
Quanying Wu ◽  
Baohua Chen ◽  
Lin Liu ◽  
Lei Chen
Keyword(s):  
Fill Factor ◽  
Optical Design ◽  
Tolerance Analysis ◽  
Field Of View ◽  
Wide Field ◽  
Aspheric Surfaces ◽  
The Monte Carlo Method ◽  
Wide Field Of View ◽  
Mirror Telescope ◽  
Telescope System

A Golay3 multi-mirror telescope (MMT) system is designed in this paper. The fill factor of the Golay3 MMT is derived from the angular resolution of the telescope. An initial configuration is established according to the paraxial optical theory. A three-element aspheric corrector group is designed and placed in the converging light cone to enlarge the field of view (FOV) of the Golay3 MMT. The tolerance analysis for each surface of the Golay3 MMT is conducted using the Monte Carlo method. The design results show the FOV of the Golay3 MMT system can be increased to 1.5° with the insertion of a three-element aspheric corrector group. The results of the tolerance analysis indicate that most tolerances are loose, while some decenter tolerances relating with the aspheric surfaces are relatively tight, but still within an acceptable range.

scholarly journals Spatial, Temporal, and Interchannel Image Data Fusion for Long-Distance Terrestrial Observation Systems

2008 ◽  
Vol 2008 ◽  
pp. 1-18 ◽  
Author(s):  
Barak Fishbain ◽  
Leonid P. Yaroslavsky ◽  
Ianir Ideses
Keyword(s):  
Data Fusion ◽  
Visual Analysis ◽  
Real Life ◽  
Super Resolution ◽  
Image Data ◽  
Video Sequences ◽  
Long Distance ◽  
Image Stabilization ◽  
Thermal Range ◽  
Observation Systems

This paper presents methods for intrachannel and interchannel fusion of thermal and visual sensors used in long-distance terrestrial observation systems. Intrachannel spatial and temporal fusion mechanisms used for image stabilization, super-resolution, denoising, and deblurring are supplemented by interchannel data fusion of visual- and thermal-range channels for generating fused videos intended for visual analysis by a human operator. Tests on synthetic, as well as on real-life, video sequences have confirmed the potential of the suggested methods.

Optical Design of Very Large Four-Mirror Systems

2007 ◽  
Vol 364-366 ◽  
pp. 1231-1236 ◽  
Author(s):  
Li Rong Zhu ◽  
Wei Min Shen
Keyword(s):  
Focal Length ◽  
Optical Design ◽  
Diffraction Limit ◽  
Field Of View ◽  
Initial Structure ◽  
Entrance Pupil ◽  
Primary Mirror ◽  
Imaging Quality ◽  
Large Aperture ◽  
Design Idea

Four-mirror systems with a very large aperture and a long focal length were investigated and designed. Their design idea is given. Through the derivation of primary aberration formula, the aberration properties were analyzed and discussed, and the method to determine its initial structure is reported. As examples, two four-mirror systems with spherical and parabolic primary mirror, 100m focal length, and 10m entrance pupil were optimally designed. Their imaging quality approaches diffraction limit within field of view of 0.4 and 0.5 degrees respectively.

Development of a New Virtual Environment System for Assembly

2006 ◽  
Vol 315-316 ◽  
pp. 556-560 ◽  
Author(s):  
G.H. Liu ◽  
Ying Xue Yao ◽  
H.Z. Zhang
Keyword(s):  
Virtual Environment ◽  
High Power ◽  
Field Of View ◽  
Wide Field ◽  
Long Distance ◽  
Spherical Cap ◽  
System A ◽  
Special Machine ◽  
Wide Field Of View ◽  
Large Spherical

In order to make the operator freely walk in virtual environment (VE), a new prototype of VE system for assembly is presented in this paper. In this system, a special machine is designed and it enables the operator to walk inside the VE in any directions over a long distance without actually leaving the physical device. Images produced by the computer are projected upon the surface of a large spherical cap screen surrounding the operator by means of a group of high power projectors. Signals provided by the position sensors attached to the operator are used by the computer to update the projected images, which provides the operator the illusion of walking freely through the virtual scenes. This VE system can acquire wide field of view and form panorama surrounding the operator, which may enhance the realistic sense of simulation.

scholarly journals TEST The Tautenburg Exoplanet Search Telescope

2008 ◽  
Vol 4 (S253) ◽  
pp. 340-342 ◽  
Author(s):  
Philipp Eigmüller ◽  
Jochen Eislöffel
Keyword(s):  
Focal Length ◽  
Variable Stars ◽  
Field Of View ◽  
Ccd Cameras ◽  
Field Identification ◽  
Main Mirror ◽  
Robotic Telescope ◽  
Telescope System ◽  
Selection Of

AbstractThe Tautenburg Exoplanet Search Telescope (TEST) is a robotic telescope system. The telescope uses a folded Schmidt Camera with a 300mm main mirror. The focal length is 940mm and it gives a 2.2° × 2.2° field of view. Dome, mount, and CCD cameras are controlled by a software bundle made by Software Bisque. The automation of the telescope includes selection of the night observing program from a given framework, taking darks and skyflats, field identification, guiding, data taking, and archiving. For the search for transiting exoplanets and variable stars an automated psf photometry based on IRAF and a lightcurve analysis based on ESO-Midas are conducted. The images and the results are managed using a PostgreSQL database.

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