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High Resolution Imagery and Slitless Spectroscopy at the Prime Focus of the CFH Telescope

Published online by Cambridge University Press:  12 April 2016

J.C. Fouéré ,
G. Lelièvre ,
J.P. Lemonier ,
G.J. Odgers ,
E.H. Richardson  and
D.S. Salmon
J.C. Fouéré
Affiliation:
Canada-France-Hawaii Telescope Corporation, P.O. 1597, Kamuela, Hawaii 96743, U.S.A.
G. Lelièvre
Affiliation:
Canada-France-Hawaii Telescope Corporation, P.O. 1597, Kamuela, Hawaii 96743, U.S.A.
J.P. Lemonier
Affiliation:
Canada-France-Hawaii Telescope Corporation, P.O. 1597, Kamuela, Hawaii 96743, U.S.A.
G.J. Odgers
Affiliation:
Canada-France-Hawaii Telescope Corporation, P.O. 1597, Kamuela, Hawaii 96743, U.S.A. Dominion Astrophysical Observatory, Victoria, B.C.
E.H. Richardson
Affiliation:
Canada-France-Hawaii Telescope Corporation, P.O. 1597, Kamuela, Hawaii 96743, U.S.A. Dominion Astrophysical Observatory, Victoria, B.C.
D.S. Salmon
Affiliation:
Canada-France-Hawaii Telescope Corporation, P.O. 1597, Kamuela, Hawaii 96743, U.S.A.

Abstract

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Direct photographic work over a large field (1°) at the prime focus of the classical Canada-France-Hawaii 3.6m telescope has been achieved with a very good image quality (less than 0.5” FWHM). The basic characteristics of the Wide-Field Corrector are presented. Our Wynne Corrector was in fact redesigned to have the last optical surface flat so that a transmission grating could be replicated thereon. This arrangement with only three optical elements locates the gratings at a maximum distance from the focal surface resulting in improved resolution over a one degree field. The C.F.H.T. grating-plus-lens, or “grens” has a brightness limit which is fainter than the Palomar Sky Survey.

Type
Section II: Spectrographs and Spectrometers
Information
International Astronomical Union Colloquium , Volume 67: Instrumentation for Astronomy with Large Optical Telescopes , 1982 , pp. 143 - 152
Copyright
Copyright © Reidel 1982

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