Charles G. Wynne 1911-1999 ============ http://www.spie.org/web/oer/january/jan00/wynne.html January 2000 Lens-design legend Charles Wynne dies Charles Gorrie Wynne, a Fellow of the Royal Society and professor of optical design at London Univ., 1969 to 1978, died on 1 October at the age of 88. Charles Wynne was the most distinguished lens designer of the postwar era. His work influenced the design of practically every lens and optical system manufactured today, including the modern camera lens, the esoteric optics used in the manufacture of silicon chips, and the giant telescopes used by astronomers. Wynne was born in Leicester, England, and won a scholarship to Wadham College, Oxford. After Oxford he returned to Leicester to work, but during WWII he went to work for Wray Optical and eventually became technical director. It was at Wray that he carried out his first work on computer-aided lens design. In the past, lens-design companies employed teams of assistants who used mechanical calculating machines to find the exact path of light rays. Wynne recognized in the 1950s that the then-new electronic computers could be used for ray tracing; however, what was needed was some means of getting the computer itself to find the best lens design, a process known as optimization. Wynne showed this could be done using a technique known as damped least squares, or DLS. His discovery revolutionized the process of lens design. Wynne's work on astronomical telescopes was particularly successful. He also served the Physical Society and the Institute of Physics. He was editor of the journal Optica Acta from 1954 to 1965; from 1975 to 1988 he was chairman of the specialist optics company I C Optical Systems. During his life he received many honors. He was elected a Fellow of the Royal Society in 1970, and he was awarded SPIE's 1999 A. E. Conrady Award. Charles Wynne is survived by his wife Jean, a son, and a daughter. Another son predeceased him. =========== July 1999 OE Reports, SPIE The A. E. Conrady Award will be presented to Charles G. Wynne, Royal Greenwich Observatory, United Kingdom, for pioneering a computer-aided method of optimizing lens designs that has become the basis of most modern optical design software packages. Wynne is also being recognized for furthering the state of the art in lens design and making many significant contributions to astronomical instrumentation. After graduating from Oxford Univ. with a Physics degree in 1935, Wynne went to work for Taylor, Taylor, and Hobson Co. in Leicester (now Taylor Hobson Pneumo) in the design-intensive environment of that company. He later went to work for the Wray Optical Company. In 1953, Wynne earned his doctorate at London Univ. and, in 1960, joined the staff of the Imperial College of Science and Technology in London as the director of their optical design group. Wynne held this post until 1978 when he reached formal retirement age. Wynne took a position at the Royal Greenwich Observatory (RGO) in Herstmonceux, although he continued as a Senior Research Fellow at the Imperial College and also as Professor Emeritus of Optical Design. When the RGO closed, Wynne moved on to the research staff of the Institute of Astronomy at the Univ. of Cambridge, where he continues to publish research papers on astronomical optics. Until recently, he was director of IC Optical Systems Ltd. Wynne was the principal founding director of this company in 1972 and its Chairman from 1975-1988. Wynne holds many patents and has published numerous papers. He has also received many awards and honors, including the Fellowship of the Royal Society, the 1971 Thomas Young Medal of the Institute of Physics, the 1979 Astronomical Society Gold medal, and the 1982 Rumford Medal of the Royal Society. ============================ The best information on the web was in Spanish, at an extensive web site. Although the translation is awkward, it is worth noting that it was accomplished with free on-line translation software. Assuming that commercial software is superior, it seems that translation software has become very useful. http://www.inaoep.mx/~rincon/wynne.html translated by http://babelfish.altavista.com/ Charles Wynne (1911-1999) Charles Wynne was born in Leicester, England. Being very young he obtained a scholarship to study physics in the University of Oxford. Once finished the degree he returned to Leicester to work like designer of lenses in the company of Taylor Hobson, in where he made original works in the design of aerial photographic lenses. They were the time of World War II, reason why the air photographs were of great importance. But late zoom lens "for television, including which they were used to film, in 1953 designed lenses", the coronation of queen Isabel II of England. Years later it worked in the Wrays company in the province of Kent, where he was the Technical Director and it initiated the field of the design of lenses with the aid of a computer. In that then one was an extremely competitive field and Charles was one of the first people in the world that attacked the problem of the optimization of the design of lenses by means of a computer. In individual it discovered the advantage to use a called technique 'minimum squares cushioned' [damped least squares] with such intention. Its technique was published in the Memories of the Royal Society in 1959. The proposed method is used practicamente in all the programs of optical design available commercially and therefore it is used in the design of virtually of all the lenses that make in the today world. Charles Wynne became well-known between the astronomers by his work on correctors of field to work in the primary center of telescopes. The field correctors are optical systems that are added to the telescope to increase the field of vision of the telescope guaranteeing that the quality of image is conserved in all that field. Also it designed telescopes of great field and correctors for the secondary centers. Between but known are the correctors designed for the telescope Anglian-Australian of 3.8m of diameter and the Isaac Newton of 2.5m of diameter. A very remarkable contribution was to demonstrate that the correctors formed by three lenses could be as efficient as those formed four lenses. The fact to eliminate a lens in the astronomical systems is of great importance since each lens introduces, inevitably, certain losses of light. Charles worked in addition in the design to the optics of the spectrographs that would work in all the great telescopes of the time. The great talent of Charles was to find solutions simple to complex problems. Some people could think that the optical design is very easy to do with all the capacity of compute that it exists at the moment. Inclusively it is possible to be gotten to think that the computer can propose one better way to us to design an optical system. The previous thing simply does not work. The designer must understand the classic theory of aberrations commercially as like the types of glass available, but first of all he requires experience. A good optical designer only uses the design programs when he is sure that there is real possibility that the optimization works. Charles was invited by P. M. S. Blackett the Group of Optical Design of the Imperial College, in London that at that time (1960) had extended the department of Physics. And continued, successful, its work in the area of the optical design by computer and its applications. In the middle of the Seventies, after its formal retirement of the Imperial College, transfer to Herstmonceux, where it worked like adviser of the Real Observatory of Greenwich. When this observatory was transferred from Sussex to Cambridge, also Charles also went away to live to Cambridge, although then he had but of 70 years. It continued working in diverse problems of optical design until a few weeks before dying, the past 1 of October. Its last article still is into the hands of the reviewers. The death of Charles marks the end of an era in which trio of the Blackett Laboratories, formed by Hopkins, Welford and Charles Wynne combined highest the individual standards with a dedication to the application of its knowledge for the benefit of the society as a whole. To a great extent this must to the effort to Blackett, that thought that in the value of contributing the society and that the application of the physical as important era as the same physics. Blackett took to the practice through the hiring and support to it of people with whom shared the same principle. The concept to apply the knowledge for the benefit of the society would have to be promoted much between the scientific community of our country. Hope Carrasco Licea & Alberto Carraminana Alonso Daily Synthesis, 19 of October of 1999 Escríbenos: bec@inaoep.mx ==================================== BIBLIOGRAPHY -------------------------------------------------------------------------------- Title: Automatic Optical Designing for Astronomy Authors: Meinel, A. B.; Schulte, D. H.; Wynne, C. G. Journal: Publications of the Astronomical Society of the Pacific, Vol. 77, No. 455, p.136 (PASP Homepage) Publication Date: 04/1965 -------------------------------------------------------------------------------- Title: Optical Design Authors: Köhler, H.; Baranne, A.; Wynne, C. G.; Meinel, A. B.; Schulte, D. H. Journal: The Construction of Large Telescopes, Proceedings from Symposium no. 27 held in Tucson, Arizona, Pasadena and Mount Hamilton, California, U.S.A., 5-12 April 1965. Edited by David Livingstone. Crawford. International Astronomical Union. Symposium no. 27, Academic Press, London, p.9 Publication Date: 00/1966 -------------------------------------------------------------------------------- Title: RITCHEY-CHRETIEN Telescopes and Extended Field Systems Authors: Wynne, C. G. Journal: Astrophysical Journal, vol. 152, p.675 Publication Date: 06/1968 -------------------------------------------------------------------------------- Title: Maksutov spectrograph cameras Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Vol. 153, p. 261 (1971) Publication Date: 00/1971 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1971MNRAS.153..261W&db_key=AST -------------------------------------------------------------------------------- Title: Five spectrograph camera designs Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Vol. 157, p. 403 (1972) Publication Date: 00/1972 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1972MNRAS.157..403W&db_key=AST -------------------------------------------------------------------------------- Title: Improved three-lens field correctors for paraboloids Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Vol. 160, p. 13P (1972) Publication Date: 00/1972 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1972MNRAS.160P..13W&db_key=AST -------------------------------------------------------------------------------- Title: Wide field Cassegrain telescopes Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Vol. 163, p. 357 (1973) Publication Date: 00/1973 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1973MNRAS.163..357W&db_key=AST -------------------------------------------------------------------------------- Title: Data for some four-lens paraboloid field correctors Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Vol. 165, p. 1P (1973) Publication Date: 00/1973 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1973MNRAS.165P...1W&db_key=AST -------------------------------------------------------------------------------- Title: A new wide-field triple lens paraboloid field corrector Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Vol. 167, p. 189-198 (1974) Publication Date: 04/1974 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1974MNRAS.167..189W&db_key=AST -------------------------------------------------------------------------------- Title: A simple wide-field Cassegrain telescope Authors: Harmer, C. F. W.; Wynne, C. G. Affiliation: AB(Royal Greenwich Observatory, Herstmonceux, Sussex, England) Journal: Royal Astronomical Society, Monthly Notices, vol. 177, Oct. 1976, p. 25P- 30P. Publication Date: 10/1976 A telescope giving an extended flat field of good imagery can be achieved by adding to a paraboloidal prime mirror a spherical convex secondary mirror and a nearly afocal spherical surfaced close doublet lens. Data are given for two designs covering an angular field of 1.5 deg in diameter at a relative aperture of f/8. -------------------------------------------------------------------------------- Title: A single-lens, small-field, paraboloid field corrector Authors: Harmer, D. L.; Wynne, C. G. Journal: The Observatory, Vol. 96, p. 239-241 (1976) Publication Date: 12/1976 -------------------------------------------------------------------------------- Title: Shorter than a Schmidt Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 180, Aug. 1977, p. 485-490. This paper is concerned with spectrograph cameras. It is shown that a system consisting of an aspheric plate, a spherical mirror and a self-achromatic lens some distance in front of the focus can be corrected for spherical aberration, coma, astigmatism, field curvature and chromatic difference of focus over a wide spectral range. Compared with a Schmidt camera of the same focal length, these systems have an overall length that is considerably shorter, by an amount that can be controlled in the design. Numerical data are given for three designs, of relative aperture f/2.5. -------------------------------------------------------------------------------- Title: Field correctors of very high performance Authors: Wynne, C. G. Journal: The Observatory, Vol. 98, p. 275-276 (1978) Publication Date: 12/1978 -------------------------------------------------------------------------------- Title: Field correctors for telescopes at better observing sites Authors: Wynne, C. G. Affiliation: AA(Royal Greenwich Observatory, Herstmonceux, Sussex; Imperial College of Science and Technology, London, England) Journal: Royal Astronomical Society, Monthly Notices, vol. 189, Oct. 1979, p. 279- 285. Publication Date: 10/1979 Abstract The results expected from the use of telescope field correctors with higher resolution than previously available at observatories with greatly improved atmospheric seeing is examined. Calculations reveal that spaced triplet correctors with spherical surfaces can reduce image spread to within 0.25 arcsec over a field of up to plus or minus 10 arcmin and a spectral range of 365-852 nm for the paraboloid mirror of the Isaac Newton 2.5-m telescope. A lens triplet consisting of a negative lens situated between two positive lenses of unequal power, or the reverse, is shown to reduce geometrical image spread to within 0.3 arcsec under the same conditions for the Ritchey-Chretien prime mirror of the Anglo-Australian 154-in. telescope. -------------------------------------------------------------------------------- Title: Field correction of a Ritchey-Chretien telescope at several focal ratios Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 193, Oct. 1980, p. 7-13. Publication Date: 10/1980 Abstract The two mirrors of a Ritchey-Chretien telescope have shapes chosen to give aplanatic imagery, generally at a focal ratio around f/8. If the secondary is replaced by one giving a materially different focal ratio, the spherical aberration of the combined system can be corrected by an appropriate mirror form, but the coma cannot also be corrected, and it may be large. It is shown that both coma and astigmatism can be corrected by the addition of an afocal thin doublet lens between the secondary mirror and the focus, together with a modification to the secondary. The analysis leads to a discriminant that determines the range of two-mirror systems for which such correction is possible. Two numerical examples are given for conversion of the 2.5-m du Pont f/7.5 telescope to work at f/15 and f/30. -------------------------------------------------------------------------------- Title: The Optics of the Achromatized UK Schmidt Telescope Authors: Wynne, C. G. Journal: ROYAL ASTRON. SOC. QUARTERLY JOURNAL V. 22, P. 146, 1981 Publication Date: 00/1981 -------------------------------------------------------------------------------- Title: Distortion of field correctors Authors: Wynne, C. G. Journal: The Observatory, vol. 101, p. 54-55 (1981) Publication Date: 04/1981 -------------------------------------------------------------------------------- Title: Spectrograph efficiency at high dispersions Authors: Wynne, C. G.; Worswick, S. P. Journal: The Observatory, vol. 103, p. 12-16 (1983) Publication Date: 02/1983 -------------------------------------------------------------------------------- Title: Ghost images on CCDs Authors: Wynne, C. G.; Worswick, S. P.; Lowne, C. M.; Jorden, P. R. Journal: The Observatory, vol. 104, p. 23-25 (1984) Publication Date: 02/1984 -------------------------------------------------------------------------------- Title: Correction of atmospheric dispersion in a converging beam Authors: Wynne, C. G. Journal: The Observatory, vol. 104, p. 140-142 (1984) Publication Date: 06/1984 -------------------------------------------------------------------------------- Title: A Dedicated Echelle Spectrometer for the Anglo-Australian Telescope Authors: Meaburn, J.; Blundell, B.; Carling, R.; Gregory, D. F.; Keir, D.; Wynne, C. G. Journal: ROYAL ASTR. SOC. MONTHLY NOT. V.210, NO.2, P.463, 1984 Publication Date: 09/1984 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1984MNRAS.210..463M&db_key=AST -------------------------------------------------------------------------------- Title: A fast relay lens for the next generation of photon-counting systems Authors: Worswick, S. P.; Wynne, C. G. Journal: The Observatory, vol. 105, p. 95-96 (1985) Publication Date: 06/1985 -------------------------------------------------------------------------------- Title: Book-Review - the Optical Papers of Isaac Newton - V.1 Authors: Shapiro, A. E.; Wynne, C. G. Journal: OBSERVATORY V.105, NO.1068/OCT, P.220, 1985 Publication Date: 10/1985 -------------------------------------------------------------------------------- Title: Atmospheric dispersion correctors at the Cassegrain focus Authors: Wynne, C. G.; Worswick, S. P. Journal: Royal Astronomical Society, Monthly Notices, vol. 220, June 1, 1986, p. 657- 670. Publication Date: 06/1986 Abstract The first-order aberration theory of an assembly of thin prisms is discussed and the results applied to derive design criteria for atmospheric dispersion correctors located in a converging beam. Two numerical examples are given of Cassegrain focus correctors for a 4.2-m f/11 and a 2.5-m f/15 telescope giving subarcsec imagery over wide spectral ranges and field angles. -------------------------------------------------------------------------------- Title: Atmospheric-dispersion correctors at prime focus Authors: Wynne, C. G. Journal: The Observatory, vol. 106, p. 163-164 (1986) Publication Date: 10/1986 -------------------------------------------------------------------------------- Title: Field correctors for short telescopes Authors: Wynne, C. G. Journal: The Observatory, vol. 107, p. 31-33 (1987) Publication Date: 02/1987 -------------------------------------------------------------------------------- Title: Atmospheric dispersion at prime focus Authors: Wynne, C. G.; Worswick, S. P. Journal: Royal Astronomical Society, Monthly Notices, vol. 230, Feb. 1, 1988, p. 457- 471. Abstract Simple atmospheric dispersion correctors suitable for use at a Cassegrain focus introduce intolerably large aberrations at prime focal ratios. An alternative system of prisms with curved optical surfaces is described, and its aberrations evaluated, which together with a slightly modified field corrector gives good correction up to 70 deg zenith distance over a 40 arcmin field. A further development of the system would make low dispersion slitless spectroscopy possible at prime focus. Numerical examples are given, designed for the f/2.5 focus of the 4.2-m William Herschel Telescope. -------------------------------------------------------------------------------- Title: Some British Advances in Optics for Astronomy Authors: Wynne, C. G. Journal: R.A.S. QUARTERLY JOURNAL V.29, NO. 1/MAR, P. 39, 1988 -------------------------------------------------------------------------------- Title: A low-dispersion survey spectrograph Authors: Wynne, C. G.; Worswick, S. P. Journal: The Observatory, vol. 108, p. 161-163 (1988) Publication Date: 10/1988 -------------------------------------------------------------------------------- Title: Wide field imaging Authors: Wynne, C. G. Affiliation: AA(Cambridge University, England) Journal: Royal Astronomical Society, Monthly Notices, vol. 236, Jan. 15, 1989, p. 47P- 50P. Abstract New types of prime focus field correctors for Ritchey-Chretien telescopes which have significantly better imaging than those presently in use are discussed. A corrector consisting of two contiguous positive lenses of relatively low power followed by separated negative and positive lenses has been applied to the f/2.7 focus of the Cerro Tololo 4-m telescope. Also considered is a 2.0-deg corrector for the Anglo- Australian 2.9-m telescope. -------------------------------------------------------------------------------- Title: Fitting spectrographs to telescopes Authors: Wynne, C. G.; Worswick, S. P. Journal: Royal Astronomical Society, Monthly Notices, vol. 237, March 1, 1989, p. 239-246. Abstract The limitations of the components of a spectrograph are reviewed. In a discussion of the devices and their limitations, consideration is given to the detectors, diffraction gratings, cameras, and collimators. Spectrographs for larger telescopes are considered as well as fiber-fed spectrographs. -------------------------------------------------------------------------------- Title: A New Form of Spectrograph Camera Authors: Wynne, C. G. Journal: R.A.S. MONTHLY NOTICES V.247, NO. 1/NOV1, P. 173, 1990 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1990MNRAS.247..173W&db_key=AST -------------------------------------------------------------------------------- Title: Wide-field collimators for spectrographs Authors: Wynne, C. G.; Escudero-Sanz, I. Journal: Royal Astronomical Society, Monthly Notices, vol. 248, Jan. 15, 1991, p. 328- 331. Abstract This paper discusses various possibilities of collimators for wide-field fiber-fed spectroscopy, that would have good correction of oblique aberration. These possible collimators include a single mirror with some form of field correction (e.g., of Schmidt or Maksutov type), a two-mirror system of Cassegrain type, purely lenticular collimators, and collimators of the Maksutov form. It is shown that an off-axis Maksutov collimator is the best type for multifiber-fed wide field spectroscopy. Such a collimator can provide a highly corrected and obstruction-free alternative to the traditional off-axis paraboloid mirrors which are only suitable for spectroscopy of small objects. Optical data are presented of an f/11 and an f/6.5 off-axis Maksutov collimators. -------------------------------------------------------------------------------- Title: Doubling spectral resolution Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 250, June 15, 1991, p. 796-801. Abstract The present paper addresses the use of diffraction gratings in general-purpose astronomic spectrographs, the grating limitations, and means of alleviating them. Grating characteristics are presented, and light loss is considered. It is concluded that, where lambda is the wavelength, s the groove spacing, m the order of diffraction, and n the reflexive index, then, (1) for given values of s and m, immersion extends diffraction to longer wavelengths than are accessible in air, and hence to higher values of R; (2) for given values of m and lambda, immersion allows the use of smaller s (finer ruled gratings) than can be used only in air at very short wavelengths, and hence an improvement of resolution; and (3) for given values of s and lambda, immersion gives access to n times higher order than in air. The procedures described offer a substantial increase of light throughput over current practice and the possibility of doubling the spectral resolution of conventional spectrographs. -------------------------------------------------------------------------------- Title: New, fast, high-performance single mirror spectrograph cameras Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 252, Sept. 1, 1991, p. 171- 176. Abstract The present study discusses the considerations that led to a new form of single-mirror spectrograph camera. Design data and performance figures are given for two f/1.2 cameras, illustrating some aspects of the versatility of these systems. The optical layout and section drawing of the single-mirror camera are presented. -------------------------------------------------------------------------------- Title: Achromatized Bowen-Vaughan telescopes Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 253, Nov. 1, 1991, p. 160- 166. Abstract The Bowen-Vaughan telescope (1973) consisting of a Ritchey-Chretien type mirror pair with a rear aspheric plate to correct the residual astigmatism of the mirrors, is limited in performance by the chromatic difference of astigmatism of the aspheric. The use of an aspheric doublet makes it possible to achieve subarcsec imagery over a wide spectral range over field diameters from 2 to 3 deg. The performance and limitations of a range of designs are described. -------------------------------------------------------------------------------- Title: Redoubling spectral resolution Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 254, Jan. 1, 1992, p. 7P- 10P. Abstract Using two immersed gratings in tandem, a spectrograph can be designed of size not much larger than a simple conventional Cassegrain spectrograph, with the same advantages of long accessible free spectral range, long slit, and multi-object capability, and in addition with spectral resolutions at least as high as are provided by an echelle spectrograph at the same slit width. -------------------------------------------------------------------------------- Title: Increasing the Efficiency and Range of Spectrographs Authors: Wynne, C. G. Journal: OPTICS IN ASTRONOMY: 32ND HERSTMONCEUX CONF.1993 P.103, 1993 -------------------------------------------------------------------------------- Title: Telecentricity in fibre-fed spectrographs Authors: Wynne, Charles G. Journal: Royal Astronomical Society, Monthly Notices, vol. 260, no. 2, p. 307-316. Publication Date: 01/1993 Abstract The paper examines the mechanism of focal degradation arising from non-telecentric illumination in a fiber-fed astronomical spectrograph. The consequent deterioration of spectrograph imagery is also considered. Data on the telecentric defect are given for several existing and projected field correctors. -------------------------------------------------------------------------------- Title: A new form of atmospheric dispersion corrector Authors: Wynne, C. G. Journal: Royal Astronomical Society, Monthly Notices, vol. 262, no. 3, p. 741-748. Publication Date: 06/1993 Abstract Earlier proposals for atmospheric dispersion correctors are briefly reviewed, and a new form described consisting of a doublet meniscus lens whose outer surfaces are concentric. The two glasses of the doublet have different dispersions, and the corrector can be tuned for different zenith distance by tipping the meniscus about the common center of its outer surfaces. This new form is simpler than earlier proposals and, in addition, in some applications it can enhance the optical performance by giving better aberration correction and reduced defect of telecentricity. Numerical data and performance figures are provided for one possible embodiment of this device. -------------------------------------------------------------------------------- Title: A Three-Lens Combined Field and Dispersion Corrector Giving Telecentric Imagery on Optics Fibres Authors: Wynne, C. G. Journal: R.A.S. MONTHLY NOTICES V.263, NO. 3/AUG1, P. 641, 1993 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1993MNRAS.263..641W&db_key=AST -------------------------------------------------------------------------------- Title: Field Imaging in Very Large Telescopes Authors: Wynne, C. G. Journal: R.A.S. MONTHLY NOTICES V.269, NO. 2/JUL15, P. L37, 1994 Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph- bib_query?1994MNRAS.269L..37W&db_key=AST -------------------------------------------------------------------------------- Title: Field correction for very large telescopes Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Volume 273, Issue 3, pp. L45-L46. Publication Date: 04/1995 Abstract Very large telescopes at present being built or planned commonly have a mirror configuration involving quite highly aberrated field imagery at the Cassegrain focus, the only focus accessible. These aberrations cause problems for instrumentation, both with and without the use of adaptive optics. The possibility of designing correctors to give wide field imagery is discussed. -------------------------------------------------------------------------------- Title: A high-resolution spectrograph for Gemini? Authors: Wynne, C. G. Journal: The Observatory, vol. 115, p. 258-261 (1995) Publication Date: 10/1995 -------------------------------------------------------------------------------- Title: Field correctors for very large telescopes Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Volume 280, Issue 2, pp. 555-558. Publication Date: 05/1996 Abstract The aberrations of astronomical telescopes are considered in terms of Seidel aberration theory, which explains why the field aberrations that limit the performance of existing large telescopes are of quite different form from those of the very large telescopes of apertures 8m and larger now being developed, and how and why quite different forms of field correctors will be required. An example is given of the design and performance of such a corrector. -------------------------------------------------------------------------------- Title: Correction of atmospheric dispersion in the infrared Authors: Wynne, Charles G. Journal: Monthly Notices of the Royal Astronomical Society, Volume 282, Issue 3, pp. 863-867. Publication Date: 10/1996 Abstract A design of atmospheric dispersion corrector for the infrared is given, suitable for the Keck 10-m telescope on Mauna Kea (altitude 4205m), to correct over the spectral range 1.0 to 2.5 mum, tuneable for stars at zenith distances 0 deg to 69.˚5. Data on the precision of the correction are also given. -------------------------------------------------------------------------------- Title: Atmospheric dispersion in very large telescopes with adaptive optics Authors: Wynne, Charles G. Journal: Monthly Notices of the Royal Astronomical Society, Volume 285, Issue 1, pp. 130-134. Publication Date: 02/1997 Abstract Current work on correcting the effects of atmospheric turbulence on telescope imagery, so as to approach the diffraction limit, requires attention to related effects to exploit it fully. In particular adaptive optics, which acts by means of a flexible mirror, is therefore colour-blind, and requires a hitherto unknown level of correction of atmospheric dispersion if it is to be used more than a few degrees from zenith. Adaptive optics can only operate over a very limited field angle and wavelength range. Fine fast auto-guiding can give substantially improved imagery, over wider field angles and wavelength range, requiring higher performance dispersion correctors than heretofore. This note describes a dispersion corrector to meet both these needs. -------------------------------------------------------------------------------- Title: Optical imaging in very large telescopes Authors: Wynne, C. G. Journal: Monthly Notices of the Royal Astronomical Society, Volume 302, Issue 4, pp. 830-832. Publication Date: 02/1999 Abstract The imaging characteristics of a telescope depend, among other things, on its size, diffraction, telescope aberrations, atmospheric seeing and dispersion, and wavelength range. The interaction of these is considered for a very large telescope, as they affect the best use of the telescope.