Far Ultraviolet Spectroscopic Explorer Spectroscopy of High-Velocity Cloud Complex C

Details Far Ultraviolet Spectroscopic Explorer Spectroscopy of High-Velocity Cloud Complex C Far Ultraviolet Spectroscopic Explorer Spectroscopy of High-Velocity Cloud Complex C

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...538l..35m&link_type=abstract

The Astrophysical Journal, Volume 538, Issue 1, pp. L35-L38.

Astronomy and Astrophysics

Astronomy

43

Galaxy: Abundances, Galaxy: General, Ism: Abundances

Scientific paper

We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the sight line toward the Seyfert 1 galaxy Markarian 876, which passes through high-velocity cloud (HVC) complex C. This sight line demonstrates the ability of FUSE to measure ionic absorption lines in Galactic HVCs. High-velocity absorption is clearly seen in both members of the O VI doublet. This is the first detection of O VI in a neutral hydrogen HVC. One component of HVC complex C is resolved in multiple Fe II lines from which we derive N(Fe II)/N(H I)=0.48 (Fe/H)solar. This value of N(Fe II)/N(H I) implies that the metallicity of complex C along this sight line may be higher than that along the Mrk 290 sight line (0.1 solar) found by Wakker et al. On the other hand, if the metallicity of complex C is also 0.1 solar along this line of sight, the observed value of N(Fe II)/N(H I) suggests there may be a significant amount of H+ along the line of sight. In any case, little, if any, iron can be depleted into dust grains if the intrinsic metallicity of complex C is subsolar. Absorption from complex C is also seen in C II, N I, and N II, and upper limits based on nondetections can be determined for Ar I, P II, and Fe III. Although molecular hydrogen in the Milky Way is obvious in the FUSE data, no H2 absorption is seen in the HVC to a limit N(H2)<2.0×1014 cm-2. Future FUSE observations of extragalactic objects behind Galactic HVCs will allow us to better constrain models of HVC origins.

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