Near-infrared camera with a HgCdTe 128 X 128 array at the CRL 1.5 M telescope

Details Near-infrared camera with a HgCdTe 128 X 128 array at the CRL 1.5 M telescope Near-infrared camera with a HgCdTe 128 X 128 array at the CRL 1.5 M telescope

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47...93h&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 47, no. 1, p. 93-104

Astronomy and Astrophysics

Astronomy

2

Arrays, Cameras, Cmos, Infrared Astronomy, Infrared Detectors, Infrared Photometry, Mercury Cadmium Tellurides, Angular Resolution, Astronomical Photometry, Fabry-Perot Spectrometers, Field Of View, Infrared Imagery, Infrared Stars, Interstellar Gas, Nonlinearity, Star Formation, Stellar Color, Stellar Magnitude, Supernova Remnants

Scientific paper

An infrared camera has been designed and constructed for the 1.5 m telescope of the Communications Research Laboratory (CRL) using a 128 x 128 HgCdTe array detector with a switched C-MOS multiplexer (TCM 1000B). The large storage capacity (3 x 107e-) of the array is advantageous for astronomical observations with long exposure in order to store many photo-electrons and under high-background conditions. We have designed a cooled optical system with a field of view of 4.2 min x 4.2 min and a resolution of 2 sec/pixel at the Nasmyth focus of the telescope. The large field of view is important for studying large extended astronomical objects. The cooled optical system and a kTC-noise limited readout circuit has achieved high efficiency of the camera system. The array detector has been found to have a small nonlinearity in the responsivity, increasing with the stored charge, which is different from a decrease of the responsivity due to a change in the capacitance of detector, which is common in arrays without an external integration capacitance. The magnitudes of infrared standard stars taken by this infrared camera at the CRL 1.5 m telescope are compared with those of the CIT (California Institute of Technology) system, in which observations were made using a single detector; the magnitude and color transformation formulas were obtained as a function of infrared colors. The difference between the two photometric systems is small in both magntiude and color. The infrared camera system has been used to take two-dimensional infrared images of galaxies, planets, and comets, and has also been combined with a Fabry-Perot spectrometer to observe interstellar gas in a star-formation region and a supernova remnant.

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