Computer Science
Scientific paper
Dec 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982msngr..30....9f&link_type=abstract
ESO Messenger, Dec. 1982, p. 9-13.
Computer Science
Absorption Spectroscopy, Interstellar Matter, Line Spectra, Spectrographs, Spectrum Analysis, Abundance, Cosmology, Deuterium, Interstellar Gas, Line Of Sight, Lithium, Magellanic Clouds
Scientific paper
Techniques for observing and analyzing the characteristics of the interstellar medium are explored. The densities of the gas and dust have been calculated to range from 1/10,000 to 1,000,000 particles/cu cm, with temperatures ranging from 10-1,000,000 K. Most of the atoms are in ground state and are most efficiently observed in terms of resonance absorption lines formed in the spectra of stars beyond them. Most absorption lines reside below 1200 A. The chemical composition of the interstellar medium can be determined by use of the line profiles fitted to theoretical Voigt profiles calculated by varying the parameters of different clouds on the line of sight, i.e., the number of clouds, their radial velocities, the b-values, and the column densities. True abundances can then be obtained by adding the contributions of different elements, then normalizing the abundances to hydrogen. Further discussion is devoted to abundance variations, the galactic halo, and the use of the coude echelle spectrograph. Sample observations of Na I, lithium, and CS(plus) ions are provided.
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