Abstract
ABSTRACT Copernicus and IUE observations of UV absorption lines of interstellar gas (IG) are reviewed. The historical context, major findings, and IG observation proposals presented in a paper by Spitzer and Zabriskie (1959) are recalled and compared with the campaigns actually undertaken and their results. Consideration is given to the performance of the satellite instruments, the observed IG depletion of most atomic species relative to hydrogen, the dominance of H2 over atomic H in dense molecular clouds, the presence of hot gas in the Galactic disk, D/H abundance ratios, neutral H distributions, and the distribution of IG in the solar vicinity. Problems encountered in interpreting UV absorption data are discussed, and the important role of the IG in the evolution of galaxies is indicated.
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