Titlebook: Infrared Detection Techniques for Space Research; Proceedings of the F V. Manno,J. Ring Conference proceedings 1972 D. Reidel Publishing Co

凝視

An Infrared Photometer for the Balloon-Borne Telescope Thisbech in October 1971 our first balloon-borne infrared photometer. By this experiment we will make a surface photometry of the night sky at 2.4 μ. I will describe in the following the main components of our project: The balloon gondola Thisbe and the 2.4 μ photometer. Finally I will give some details a

defuse

Measurements of the Atmospheric Background Emission Between 10μ and 100 μfrared astronomy programme at University College London. The instrument used was a Michelson interferometer, flown at night on a balloon from Palestine, Texas during August 1969. Details of the instrument and the methods of data reduction and calibration are given elsewhere [1].

災(zāi)禍

Paradox

Infrared Rocket Astronomyscuration of the Earth’s atmosphere. Ground-based near infrared astronomy could be carried out within certain partial windows: i.e. from 2.1 μ to 2.4 μ, 3.5 μ to 4.0 μ, 4.6 μ to 4.7 μ, 8–13 μ, and 20–25 μ. The region from 25 μ to 2 mm is completely opaque and measurements have to be carried out from

連詞

ARCHE

Infrared Detectors. Survey of the Present State of the Arte present achievements in the field of bolometers, photoconductors and Josephson junctions. We also evaluate potential use of heterodyne detection applied to both spectroscopy and wide-band detection. Finally, some attention is paid to exotic types of detectors which may become of interest in a near

Schlemms-Canal

lymphoma

兇兆

Analogy