Development of Cryogenic Camera

Details Development of Cryogenic Camera Development of Cryogenic Camera

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..395a&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Astronomy and Astrophysics

Astronomy

Scientific paper

The sensitivity of the ground-based infrared observation is limited by thermal emission from the telescope and the atmosphere. At the wavelengths longer than 2.5 μm, the dominant emission comes from the telescope and can be reduced by cooling it down. We have developed Cryogenic Camera, which is a small Cassegrain telescope in a cryostat. Its effective diameter is 22 cm, and it uses a 256 x 256 InSb detector by SBRC, with a pixel scale of 5.6 arcsec, and consequently a field coverage of 24 x 24 arcmin2. In the test observations at Nagoya University in 1999 April, the background brightness was measured to be 5.9 mag/arcsec2 at 3.6 μm. Although the observations were made under the high sky-background condition in Nagoya, this was fainter by > 1 mag/arcsec2 than those obtained with conventional telescopes at good astronomical sites. The limiting surface brightness at 3.6 μm for one second integration was 1σ=11.6 mag/arcsec2, but this was affected by high system noise at that time. With the reduction of the noise and under good sky conditions, we expect the limiting surface brightness 1σ=13.7 mag/arcsec2.

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