Kinematics, Ionization, and Abundances of the High Velocity Clouds Toward PG 1116+215

Details Kinematics, Ionization, and Abundances of the High Velocity Clouds Toward PG 1116+215 Kinematics, Ionization, and Abundances of the High Velocity Clouds Toward PG 1116+215

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aspc..348..394g&link_type=abstract

Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE ASP Conference Series, Vol. 348, Proceedings of the Confe

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present ultraviolet spectra of the high Galactic latitude sight-line toward PG 1116+215 from FUSE and HST/STIS. The high resolution (20 km/s for FUSE, 6.5 km/s for STIS) and broad wavelength coverage (905--2820 Å) allow us to examine the detailed kinematics, ionization, and abundances of the high velocity cloud (HVC) at vLSR=+184 km s-1. We detect a wide range of ions, including H I, O I, and O VI. The fortuitous detection of both O I and H I in this isolated HVC allows for a robust, albeit uncertain, metallicity constraint of ˜0.2 solar for the neutral gas. From comparison of the O VI, Si II, and O I column densities, we estimate that ionized gas dominates neutral gas by at least 10:1. We suggest a scenario where clumps of gas, which produce low ions, are interacting with a low-density medium, such as the Galactic halo or corona, which produces the high ions in the interaction region. A simple photoionization model of the neutral and low ions implies densities of at least 2 × 10-3 cm-3 for the low ionization gas.

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