Research on Spectroscopy, Opacity, and Atmospheres

Details Research on Spectroscopy, Opacity, and Atmospheres Research on Spectroscopy, Opacity, and Atmospheres

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996sao..repts....k&link_type=abstract

Technical Report, Smithsonian Astrophysical Observatory Cambridge, MA United States

Astronomy and Astrophysics

Astrophysics

Line Spectra, Atomic Spectra, Astronomical Spectroscopy, Stellar Spectra, Hyperfine Structure, Spectrum Analysis, Data Bases

Scientific paper

The main accomplishment was the merging of all the atomic line data into one wavelength-sorted list that is simple to use. We have combined all the atomic files from a CDROM into 534,910 line files GFALL.DAT and GFELEN.DAT. These are the data we use to compute spectra. They are not up to date. References are given in GFALL.REF or GFELEK.REF. There are no references after 1988, and for light elements there are no references after 1979. One new development is the inclusion of hyperfine splitting for the iron group elements using hyperfine data from the literature through 1993. The data are very incomplete. We have supplied a program for splitting the line list for a species. It reads the hyperfine and isotopic splitting parameters for levels and computes the splittings whenever those levels appear. Lines with no splitting data are copied untouched. Because Sc, Mn, and Co are monoisotopic, only the hyperfine splittings are needed. Since 51V is much more abundant than 50V, the isotope shifts are small for 51V, and we approximate V with 51V. GFALLHYP.DAT has 754,946 lines including hyperfine Sc I, V I, Mn I, and Co I.

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