28 December 1989 Role Of UV Stellar Intensity Measurements In Atmospheric Transmissions Modelling
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Abstract
An 18-in. Cassegrain telescope and UV imaging system is used to observe and record starlight in the wavelength range 3000-3700 A . Such observations provide a real-time sampling of the atmosphere, allowing an accurate study of remote UV sources of unknown intensity. The spatial dependence for the trans-mission of radiation through the atmosphere has been calculated using the LOWTRAN 6 computer code, and the results are compared to data from various UV-emitting stars. Variations in the atmosphere are seen to strongly depend on aerosol concentration which affects meteorological range. Ground-level photometer measurements of extinction coefficients are extrapolated to yield atmospheric visibility profiles for our observation point.
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A. V. Dentamaro, C. G. Stergis, V. C. Baisley, "Role Of UV Stellar Intensity Measurements In Atmospheric Transmissions Modelling", Proc. SPIE 1158, Ultraviolet Technology III, (28 December 1989); doi: 10.1117/12.962553; https://doi.org/10.1117/12.962553
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