Proceedings Paper
Role Of UV Stellar Intensity Measurements In Atmospheric Transmissions Modelling| Format | Member Price | Non-Member Price |
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Paper 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.
Paper Details
Date Published: 28 December 1989
PDF: 11 pages
Proc. SPIE 1158, Ultraviolet Technology III, (28 December 1989); doi: 10.1117/12.962553
Published in SPIE Proceedings Vol. 1158:
Ultraviolet Technology III
Robert E. Huffman, Editor(s)
PDF: 11 pages
Proc. SPIE 1158, Ultraviolet Technology III, (28 December 1989); doi: 10.1117/12.962553
Show Author Affiliations
A. V. Dentamaro, Science Applications International Corporation (United States)
C. G. Stergis, Geophysics Laboratory (AFSC) (United States)
C. G. Stergis, Geophysics Laboratory (AFSC) (United States)
V. C. Baisley, Geophysics Laboratory (AFSC) (United States)
Published in SPIE Proceedings Vol. 1158:
Ultraviolet Technology III
Robert E. Huffman, Editor(s)
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