Optical design of an atmospheric dispersion compensator for the DAG-AO system

2021 ◽  
Author(s):  
Audrey T. Bouxin ◽  
Laurent Jolissaint ◽  
Onur Keskin ◽  
Cahit Yesilyaprak ◽  
Paolo Spanò
Keyword(s):  
Optical Design ◽  
Atmospheric Dispersion ◽  
Dispersion Compensator

Optical design of a broadband atmospheric dispersion corrector for MAVIS

2020 ◽  
Author(s):  
Davide Greggio ◽  
Christian Schwab ◽  
Demetrio Magrin ◽  
Simone Di Filippo ◽  
Valentina Viotto ◽  
...  
Keyword(s):  
Optical Design ◽  
Atmospheric Dispersion

scholarly journals Implementation and Use of Wide Fields in Future Very Large Telescopes

1984 ◽  
Vol 78 ◽  
pp. 549-562 ◽  
Author(s):  
J.R.P. Angel
Keyword(s):  
High Efficiency ◽  
Optical Design ◽  
Atmospheric Dispersion ◽  
General Purpose ◽  
Full Potential ◽  
Large Area ◽  
Full Field ◽  
Drift Scan ◽  
Large Telescopes ◽  
Ccd Arrays

AbstractThe full potential of the next generation of larger telescopes will be realized only if they have well instrumented large fields of view. Scientific problems for which very large ground-based optical telescopes will be of most value often will need surveys to very deep limits with imaging and slitless spectroscopy, followed by spectroscopy of faint objects taken many at once over the field. Improved instruments and detectors for this purpose are being developed. Remotely positioned fibers allow the coupling of light from many objects in the field to the spectrograph slit. CCD arrays, operated in the TDI or drift scan mode, will make large area detectors of high efficiency that may supercede photographic plates. An ideal telescope optical design should be based on a fast parabolic primary, have a field of at least 1° with achromatic images < 0.25 arcseconds and have provision for dispersive elements to be used for slitless spectroscopy and compensation of atmospheric dispersion over the full field. A good solution for a general purpose telescope that can satisfy these needs is given by a three element refractive corrector at a fast Cassegrain focus. A specialized telescope dedicated to sky surveys, with better image quality and higher throughput than presently available, might be built as a scaled up Schmidt with very large photographic plates. Better performance in most areas should be obtained with a large CCD mosaic detector operated in the drift scan mode at a telescope with a 2-mirror reflecting corrector.

Design and implementation of an atmospheric dispersion compensator/corrector for the Gemini multi-object spectograph

2003 ◽  
Author(s):  
Kei Szeto ◽  
Christopher L. Morbey ◽  
Christopher J. Mayer ◽  
David Crampton ◽  
J. Murray Fletcher ◽  
...  
Keyword(s):  
Atmospheric Dispersion ◽  
Design And Implementation ◽  
Dispersion Compensator

scholarly journals Antarctica – a case for 3D-spectroscopy

2006 ◽  
Vol 2 (14) ◽  
pp. 707-708
Author(s):  
Andreas Kelz
Keyword(s):  
Atmospheric Dispersion ◽  
Spectrograph Slit ◽  
Dispersion Compensator ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

DS or Integral-Field Spectroscopy (IFS) provides multiple spectra for each point of a 2-D field, rather than along a narrow, 1-D spectrograph slit only. Therefore, IFS does not require very accurate telescope pointing, nor do pre-assumptions about slit or aperture sizes have to be made. It avoids any ‘slit-losses’ due to seeing or atmospheric dispersion, which eliminates the need for any parallactic alignment or a dispersion compensator (see Fig. 1).

Charles Gorrie Wynne. 18 May 1911 – 1 October 1999

2001 ◽  
Vol 47 ◽  
pp. 497-514
Author(s):  
Jonathan Maxwell ◽  
Prudence M.J.H. Wormell
Keyword(s):  
Bubble Chamber ◽  
Optical Design ◽  
Atmospheric Dispersion ◽  
Working Life ◽  
High Energy ◽  
Formative Period ◽  
Computer Assisted ◽  
Original Research ◽  
Lens Design ◽  
Large Telescopes

Charles Gorrie Wynne dedicated his professional life to optical design and became a principal figure in the international optical design community. When he died, he was optical consultant to the Institute of Astronomy in Cambridge and Emeritus Professor of Optical Design at Imperial College. Although nearly 90 years old he worked several days a week in the Institute of Astronomy until a few months before he died. He was elected to Fellowship of The Royal Society in 1970. Wynne's expertise was in the field of optical instrument design, particularly lens design. Among lens designers he is best known for his effective theories of lens design, his elegant and ambitious lens designs, and particularly his invention of a very successful method of computer-assisted lens design, based on the method of least squares. Among astronomers he is known for what is almost a monopoly of designs for field–widening optics for large telescopes, and also for a series of scientifically elegant spectrographs and atmospheric dispersion correctors. With microcircuit manufacturers he is famous for his work on the Wynne–Dyson catadioptric relay printer for microcircuit production. By high–energy physicists he is known as the designer of bubble–chamber optics; finally, he is known by his assistants and his students as their professional mentor. During the formative period of Charles Wynne's working life, optical design was performed almost exclusively behind the closed doors of optical factories. The optical designers in those factories traditionally led a monastic working life, closeted with a few close colleagues and assistants, grappling with the extensive numerical calculations that optical design involves. During the period of his career when he worked in this way, he managed to combine this type of working life with creative original research into new types of lens system and new methods of lens design.

Use of the Magnetostatic Analogue In Electromagnetic Lens Engineering

1970 ◽  
Vol 28 ◽  
pp. 360-361
Author(s):  
John W. Coleman
Keyword(s):  
Boundary Conditions ◽  
High Performance ◽  
Force Fields ◽  
Optical Design ◽  
Direct Conversion ◽  
Design Engineering ◽  
Design Data ◽  
Scalar Potentials ◽  
Geometric Elements ◽  
At Will

In the design engineering of high performance electromagnetic lenses, the direct conversion of electron optical design data into drawings for reliable hardware is oftentimes difficult, especially in terms of how to mount parts to each other, how to tolerance dimensions, and how to specify finishes. An answer to this is in the use of magnetostatic analytics, corresponding to boundary conditions for the optical design. With such models, the magnetostatic force on a test pole along the axis may be examined, and in this way one may obtain priority listings for holding dimensions, relieving stresses, etc..The development of magnetostatic models most easily proceeds from the derivation of scalar potentials of separate geometric elements. These potentials can then be conbined at will because of the superposition characteristic of conservative force fields.

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