Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6203s&link_type=abstract
American Astronomical Society, DPS meeting #38, #62.03; Bulletin of the American Astronomical Society, Vol. 38, p.605
Astronomy and Astrophysics
Astronomy
Scientific paper
We have constructed synthetic solar spectra for the 2.5 - 3.0 μm, 4.1 - 4.4 μm, and 5.1 - 7.7 μm ranges using Voigt line profiles, and with solar line identifications compiled by Geller (1992), who derived solar line positions and intensities from contaminated high-resolution solar spectra obtained by ATMOS (Atmospheric Trace Molecule Spectroscopy), a spaceborne observatory. Because the ATMOS spectra in these wavelength ranges are contaminated by absorption lines of molecules existing in Earth's high-altitude atmosphere, the direct use of this high-resolution solar spectra has been inconvenient for planetary scientists. We compared the synthetic solar spectra with the ATMOS spectra, and obtained satisfactory fits with the exception of a few abnormal lines. From the satisfactory comparisons, we were able to determine Voigt line parameters for each solar line. These synthetic solar spectra will be useful to eliminate solar continua from spectra of planetary objects to extract their own spectral characteristics.
Reference
Geller, M., 1992, A High-Resolution Atlas of the Infrared Spectrum of the Sun and the Earth Atmosphere from Space, Vol. III. Key to Identification of Solar Features, NASA Reference Pub. 1224.
Jang Minsung
Kim Jongsoo
Kim Seongcheol
Seo Haing Ja
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