Optical design of the Magellan Project 6.5-meter telescope

Stephen A. Shectman

doi:10.1117/12.176223

1 June 1994 Optical design of the Magellan Project 6.5-meter telescope

Stephen A. Shectman

Proceedings Volume 2199, Advanced Technology Optical Telescopes V; (1994) https://doi.org/10.1117/12.176223
Event: 1994 Symposium on Astronomical Telescopes and Instrumentation for the 21st Century, 1994, Kailua, Kona, HI, United States

Abstract

The Magellan Project 6.5-meter telescope includes focal stations at both Cassegrain and Nasmyth locations. Instruments which use the f/15 infrared secondary will be mounted at the Cassegrain position. The Nasmyth foci will be fed by an f/11 Gregorian secondary. Rapid changes between the Cassegrain and Nasmyth configurations will be accomplished using a flip-tertiary diagonal mirror. The tertiary mirror turret includes a two-element field corrector and atmospheric dispersion compensator for use with the Gregorian secondary. The turret and the tertiary rotate in order to direct the light to one of 5 Gregorian focal stations, as well as to select or to bypass the field corrector/ADC for any focal station. The optical design of the corrector produces a 30 arc-min diameter field. The Gregorian focal ratio has been chosen to accurately match the field curvature of a particular collimator design, which is the first part of an imaging spectrograph with a 30 arc-min field of view. A variety of cameras will be used with this spectrograph. The wide-field camera should cover the entire field of view with a typical rms image diameter of 0.5 arc-sec. The high-resolution camera should cover the central 15 arc-min with a typical rms image diameter of 0.1 arc-sec.

Citation Download Citation

Stephen A. Shectman "Optical design of the Magellan Project 6.5-meter telescope", Proc. SPIE 2199, Advanced Technology Optical Telescopes V, (1 June 1994); https://doi.org/10.1117/12.176223

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