Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990spie.1235...63s&link_type=abstract
IN: Instrumentation in astronomy VII; Proceedings of the Meeting, Tucson, AZ, Feb. 13-17, 1990 (A91-29601 11-35). Bellingham, WA
Astronomy and Astrophysics
Astronomy
4
Charge Coupled Devices, Cryogenic Equipment, Data Reduction, Electronic Control, Infrared Photography, Mercury Cadmium Tellurides, Cameras, Multiplexing, Near Infrared Radiation, Pixels
Scientific paper
A large area, near-infrared (1-2.5-micron) camera system was constructed for use at the prime focus of the Wyoming Infrared Observatory (WIRO) 2.3-m telescope. The detector is a 64 x 64 element HgCdTe array. A microprocessor-based control board residing on the dewar clocks the CCD multiplexer, controls the double-correlated sampling, and digitizes the detector signal. All voltage levels and clocking sequences can be adjusted by software in real time. The data acquisition computer communicates with the control board over a modified RS-232 link at an adjustable rate (usually 50 kilobaud). This allows virtually any computer to be used for data acquisition with a minimum of difficulty. The optics are optimized for the study of extended sources of low surface brightness, with maximum optical throughput. The f/2 primary is followed by a liquid-nitrogen-cooled Wynne corrector and two cold-filter wheels with a capacity of 12 individual filters and a 90-degree CVF segment. The positions of the lens, the instrument, and the filter wheels are adjusted by stepper motors. The plate scale is 2.06 arcseconds per pixel.
Johnson Paul E.
Spillar Earl
Warren David
Wenz Michael
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