Physics – Optics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.0908h&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #09.08; Bulletin of the American Astronomical Society, Vol. 24, p.741
Physics
Optics
Scientific paper
The Columbus Project telescope is a 2 x 8.4 meter binocular instrument being built by the University of Arizona and the Osservatorio Astrofisico di Arcetri. Dual 8.4 meter borosilicate honeycomb primary mirrors provide an equivalent collecting area of 11.8 meters. With a focal ratio of F/1.14, these primaries will permit a very compact and stiff telescope structure. The combined focus provides an interferometric baseline of 22.8 meters on a common mount. The phased focus provides a coherent field-of-view up to 6 arcminutes in diameter at F/33. In addition to a central focus for interferometry, the telescope will be instrumented with dual Cassegrain focal stations at F/5 and F/15. The F/5 foci will be optimized for wide field work in the optical and near-infrared. The 1.96 m diameter secondaries provide a naked Cassegrain focus at F/5.2. A three-element refractive corrector provides a 50 arcminute field-of-view at F/5.4. This wide field will be used for multiobject spectroscopy as well as wide field imaging and long-slit spectroscopy. The F/15 foci will be optimized for work at mid- and thermal infrared wavelengths with approximately a 10 arcminute field-of-view. The infrared foci will be used for imaging and spectroscopy over a wide wavelength range. The 0.74 m diameter secondaries will have chopping and rapid guiding capabilities. Adaptive optics will also play a key role in the telescope operation. Tertiary flats will provide bent Cassegrain focal stations. Secondaries which are not in use will be stored in the center of the telescope structure allowing for rapid interchange during the night. The error budget for the optics and the telescope will attempt to match the wavefront provided by an r_0 = 45 cm atmosphere.
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