The interstellar band at lambda 4430 A and the abundance of interstellar iron, titanium, and molecular hydrogen

Details The interstellar band at lambda 4430 A and the abundance of interstellar iron, titanium, and molecular hydrogen The interstellar band at lambda 4430 A and the abundance of interstellar iron, titanium, and molecular hydrogen

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..84..505z&link_type=abstract

Astrophysics and Space Science, vol. 84, no. 2, June 1982, p. 505-517.

Astronomy and Astrophysics

Astrophysics

1

Abundance, Astronomical Spectroscopy, Hydrogen Clouds, Iron, Titanium, Cosmic Dust, Interstellar Matter, Visible Spectrum

Scientific paper

For the direction to a number of stars the depletion of interstellar gaseous iron and titanium as well as the relative abundance of molecular hydrogen and the strength of the interstellar band at A 4430 A were determined by different authors and can be found in the literature. In this paper it is shown that the difference (A~ - A~0) is a more reliable measurement of the column density of 4430 A absorbers than the usually used central depth, A~, because the positive value A~0 of A~ for E(B - V) = 0, i.e. the intercept with the A~ axis of a least-squares fit to the observed A~ vs E(B - V) data, is with a high probability not caused by an interstellar effect. There was no correlation found between the interstellar depletion of iron and titanium, respec- tively, and (A~ - A~0), whereas a tendency exists that with increasing relative molecular hydrogen abundance the number of 4430 A absorbers per hydrogen atom decreases. If the carriers of the 4430 A absorbers are interstellar grains, then these grains must be altered during the same process in which molecular hydrogen is built. The found correlation is also compatible with the assumption that the 4430 A absorber is related to an interstellar gaseous species

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