Abundances of interstellar atoms from ultaviolet absorption lines

Details Abundances of interstellar atoms from ultaviolet absorption lines Abundances of interstellar atoms from ultaviolet absorption lines

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...301..355j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 1, 1986, p. 355-379.

Astronomy and Astrophysics

Astronomy

179

Absorption Spectra, Abundance, Interstellar Matter, Spectral Line Width, Ultraviolet Astronomy, H Ii Regions, Metallicity, Space Density, Spectral Correlation

Scientific paper

The equivalent widths of interstellar absorption lines of Mg II, P II, Cl I and II, Mn II, Fe II, Cu II, and Ni II, obtained in a Copernicus survey of Bohlin et al (1983) have been analyzed to yield column densities along the lines of sight. The measured depletions are clearly correlated with nH, the mean hydrogen column density along the line of sight. Depletions also seem to be weakly correlated with various ratios of hydrogen to extinction by dust grains and also variations of extinction with wavelength, although part of these effects are a secondary result of the correlation with nH. The apparent coupling of depletion to the mean density are interpreted in terms of an idealized model due to Spitzer (1985), where each element has one value of depletion in the low-density, warm, neutral gas and an enhanced, different value in cold clouds. The difference of apparent depletions for Mg, P, Cl, Mn, and Fe between warm and cold clouds averages 0.44 + or - 0.12 (rms) dex, and, after an allowance for observational errors is made, the scatter of individual depletions from the overall trend predicted by method is only about 0.10 dex. The identification of the observed apparent depletions with actual ones, while very likely, is not entirely secure, because of the possible presence of highly saturated compoents with very narrow profiles and the possible contamination of the results by H II regions.

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