Intersstellar absorption lines between 2000 and 3000 A in nearby stars observed with BUSS

Details Intersstellar absorption lines between 2000 and 3000 A in nearby stars observed with BUSS Intersstellar absorption lines between 2000 and 3000 A in nearby stars observed with BUSS

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...157..119d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 157, no. 1, March 1986, p. 119-128. Research supported by the Koninklijke Nede

Astronomy and Astrophysics

Astronomy

42

Astronomical Spectroscopy, Balloon-Borne Instruments, Interstellar Gas, Ultraviolet Astronomy, Absorption Spectra, Abundance, Hydrogen Clouds, Line Spectra, Metals, Nebulae

Scientific paper

Spectra obtained between 2000 and 3000 A with the Balloon Borne Ultraviolet Spectrophotometer (BUSS) payload were examined for interstellar absorption lines. In bright stars, with spectral types between O9V and F5V, such lines were measured of Mg I, Mg II, Cr II, Mn II, Fe II and Zn II, with Cr II and Zn II data of especially high quality. Column densities were derived and interstellar abundances were determined for the above species. It was found that metal depletion increases with increasing E(B-V); Fe was most affected and Zn showed a small depletion for E(B-V) greater than 0.3 towards Sco-Oph. The metal column densities, derived for Alpha-And, Kappa-Dra, Alpha-Com, Alpha-Aql, and 29 Cyg were used to infer N(H I). It was shown that the ratio of Mg I to Na I is instrumental in determining the ionization structure along each line of sight. The spectra of Aql stars confirms the presence of large gas densities near Alpha-Oph. Moreover, data indicated that the Rho-Oph N(H I) value needs to be altered to 35 x 10 to the 20th/sq cm, based on observed ion ratios and analysis of the Copernicus L-alpha profile.

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