SOFIA primary mirror assembly: structural properties and optical performance

2003 ◽  
Author(s):  
Hermann Bittner ◽  
Matthias Erdmann ◽  
Peter Haberler ◽  
Karl-Heinz Zuknik
Keyword(s):  
Structural Properties ◽  
Optical Performance ◽  
Primary Mirror

A Study on the Adhesive Effects on the Optical Performance of the Primary Mirror System of a Satellite Camera

2007 ◽  
Vol 51 (6) ◽  
pp. 1901 ◽  
Author(s):  
Yu-Deok Seo ◽  
Hyun-Jung Kim ◽  
Sung-Kie Youn ◽  
Seung-Hoon Lee ◽  
Deog-Gyu Lee ◽  
...  
Keyword(s):  
Mirror System ◽  
Optical Performance ◽  
Primary Mirror

scholarly journals The Instruments of H.E. Dall

1988 ◽  
Vol 98 ◽  
pp. 46-47
Author(s):  
E.J. Hysom
Keyword(s):  
Numerical Aperture ◽  
Science Museum ◽  
Optical Performance ◽  
World War ◽  
Primary Mirror ◽  
World War 2 ◽  
Insufficient Time ◽  
Cassegrain Telescope ◽  
Working Distance ◽  
Prolate Ellipsoidal

In 1926 Horace Dall commenced optical work, with interests covering both microscopes and telescopes. Soon (1928), he was making solid eyepieces of the Tolles type. Eventually he developed skills in making lenses of the smallest size to be incorporated into microscope objectives of the highest numerical aperture; this culminated in an objective with a N.A. of 1.92 (a record). The lenses were jewelled elements worked with diamond dust. During World War 2 he repaired all the microscope lenses damaged in the U.K. that had originated with the German firm of Leitz.Horace Dall had an exceptionally inventive mind – and was so active in developing his ideas that he had insufficient time to formally write them up, hence much of his work remains unpublished. He did, however, keep extensive notebooks of his researches into optics. These, along with many prototypes, are now in the custody of the Science Museum, London. Combining his interests in travel, optics, and astronomy, Dall developed a number of portable, ultra-lightweight telescopes. He discovered that by incorporating what is in effect a long working distance, low-power microscope with a Cassegrain telescope he had an instrument with several advantages. The image was erect, the secondary small, and by use of a suitably placed internal stop, sky-flooding was eliminated without the use of shade tubes. Always looking for improvements in optical performance he hit on the idea of modifying the classical Cassegrain telescope by employing a prolate ellipsoidal primary mirror with a spherical secondary: independently discovered by Kirkham in the U.S.A. the type is now universally known as the Dall-Kirkham.

scholarly journals An Optical Design for an Antarctic 2 m Telescope with a Near IR Imager

2002 ◽  
Vol 19 (3) ◽  
pp. 301-305 ◽  
Author(s):  
P. R. Gillingham
Keyword(s):  
Optical Design ◽  
Detector Array ◽  
Optical Performance ◽  
Primary Mirror ◽  
Low Level ◽  
Near Ir ◽  
Field Curvature ◽  
Ir Imager ◽  
Extraneous Radiation

AbstractA study has been made of the optical performance to be expected from an Antarctic Ritchey Chrétien telescope with a 2 m diameter primary mirror imaging directly onto a detector array in the K and L infrared windows. Near diffraction limited performance is provided across a flat 30 arcmin diameter field by compensating the astigmatism and field curvature with a meniscus lens which also serves as the Dewar window. With baffling inside and Narcissus mirrors outside the Dewar, extraneous radiation can be kept to a low level.

On the Use of Electrostrictive Actuators in Recovering the Optical Performance of the Hubble Space Telescope

1994 ◽  
Vol 360 ◽  
Author(s):  
James L. Fanson
Keyword(s):  
Hubble Space Telescope ◽  
Spherical Aberration ◽  
Wide Field ◽  
Optical Performance ◽  
Space Telescope ◽  
Jet Propulsion ◽  
Primary Mirror ◽  
Optical Correction ◽  
Active Mirror ◽  
Multilayer Actuators

AbstractThis paper describes the development of a space qualified active mirror—the Articulating Fold Mirror—which forms part of the scheme for recovering the optical performance of the Hubble Space Telescope. Three Articulating Fold Mirrors are incorporated into the optical train of the Jet Propulsion Laboratory's Wide Field and Planetary Camera-2, which was installed into Hubble by astronauts in December, 1993. Each Articulating Fold Mirror utilizes six electrostrictive ceramic multilayer actuators to precisely position a mirror in tip and tilt in order to correct the spherical aberration of the Hubble Space Telescope's primary mirror. Flight qualification aspects of the electrostrictive actuators are described. Pre- and postrepair images from the Wide Field and Planetary Camera, showing the effect of the optical correction, are presented.

scholarly journals Design and Optimization for Mounting Primary Mirror with Reduced Sensitivity to Temperature Change in an Aerial Optoelectronic Sensor

Sensors ◽  
2021 ◽  
Vol 21 (23) ◽  
pp. 7993
Author(s):  
Meijun Zhang ◽  
Qipeng Lu ◽  
Haonan Tian ◽  
Dejiang Wang ◽  
Cheng Chen ◽  
...  
Keyword(s):  
Surface Shape ◽  
Shape Error ◽  
Temperature Decrease ◽  
Mirror Surface ◽  
Optical Performance ◽  
Uniform Temperature ◽  
Primary Mirror ◽  
Optoelectronic Sensor ◽  
Thermal Adaptability

In order to improve the image quality of the aerial optoelectronic sensor over a wide range of temperature changes, high thermal adaptability of the primary mirror as the critical components is considered. Integrated optomechanical analysis and optimization for mounting primary mirrors are carried out. The mirror surface shape error caused by uniform temperature decrease was treated as the objective function, and the fundamental frequency of the mirror assembly and the surface shape error caused by gravity parallel or vertical to the optical axis are taken as the constraints. A detailed size optimization is conducted to optimize its dimension parameters. Sensitivities of the optical system performance with respect to the size parameters are further evaluated. The configuration of the primary mirror and the flexure are obtained. The simulated optimization results show that the size parameters differently affect the optical performance and which factors are the key. The mirror surface shape error under 30 °C uniform temperature decrease effectively decreased from 26.5 nm to 11.6 nm, despite the weight of the primary mirror assembly increases by 0.3 kg. Compared to the initial design, the value of the system’s modulation transfer function (0° field angle) is improved from 0.15 to 0.21. Namely, the optical performance of the camera under thermal load has been enhanced and thermal adaptability of the primary mirror has been obviously reinforced after optimization. Based on the optimized results, a prototype of the primary mirror assembly is manufactured and assembled. A ground thermal test was conducted to verify difference in imaging quality at room and low temperature, respectively. The image quality of the camera meets the requirements of the index despite degrading.

The optical performance test of lightweight primary mirror of space Cassegrain telescope

2013 ◽  
Author(s):  
Wei-Cheng Lin ◽  
Shenq-Tsong Chang ◽  
Ting-Ming Huang ◽  
Ming-Ying Hsu ◽  
Yu-Chuan Lin
Keyword(s):  
Performance Test ◽  
Optical Performance ◽  
Primary Mirror ◽  
Cassegrain Telescope

The Telescope Primary Mirror Isostatic Mount Bonding Position Analysis

2013 ◽  
Vol 284-287 ◽  
pp. 2812-2815
Author(s):  
Ming Ying Hsu ◽  
W.C. Lin ◽  
Chia Yen Chan ◽  
C. F. Ho ◽  
S.T. Chang ◽  
...  
Keyword(s):  
Finite Element ◽  
Surface Deformation ◽  
Gravity Force ◽  
Mirror Reflection ◽  
Mirror Surface ◽  
Optical Performance ◽  
Primary Mirror ◽  
Position Errors ◽  
Result Show ◽  
Alignment Process

The telescope primary mirror Isostatic Mount (ISM) design is an important issue for optical performance. The ISM bonding position will affect the telescope performance. The primary mirror reflection surface is parallel with gravity force during telescope alignment process. Thus, the distance between ISM geometry center and primary mirror center of gravity will lead mirror surface deformation. The ISM mounting mainly aberration is astigmatism at mirror surface. This study is applied Finite Element (FEM) simulate mirror surface deformation and using Zernike polynomial fitting the mirror surface aberration. The simulation result show the ISM bonding at mirror neutral plane the aberration will minimum at 1G gravity. The ISM bonding position errors also affect aberration distribution.

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