Other
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.0611s&link_type=abstract
American Astronomical Society, 195th AAS Meeting, #06.11; Bulletin of the American Astronomical Society, Vol. 31, p.1375
Other
Scientific paper
Far Ultraviolet Spectroscopic Explorer observations of stars in the Magellanic Clouds, AGNs, and QSOs are analyzed to obtain information about O VI 1031.93 and 1037.62 Angstroms absorption occurring over long paths through the Milky Way halo. With 113.87 eV required to ionize O V, O VI is the best diagnostic of the hot interstellar medium at wavelengths > 912 Angstroms. O VI peaks in abundance at T 3*E5 K for gas in collisional ionization equilibrium and is an excellent tracer of cooling hot gas. The FUSE observations were obtained prior to telescope focusing and have spectral resolutions of 15,000, or 20 km /sec. The AGNs and QSOs studied include ESO141-055, H1821+643, VIIZw118, PG0804+761, PG0052+251, Mrk876, and several others scheduled for November and December 1999. The O VI line at 1037.62 Angstroms is often blended with absorption from C II* and the H2 (5,0) R(1) and P(1) lines. However, the O VI 1031.93 Angstroms line is usually free of blending. Since the O VI 1031.93 Angstroms halo gas absorption is relatively broad compared to the instrumental resolution, the measurements provide reliable information about the O VI column density and the kinematics of the gas. The FUSE observations are combined with earlier O VI results from the Copernicus Satellite and from ORFEUS to obtain measures of the general distribution of O VI in the halo of the Galaxy, the scale height of O VI, the degree of irregularity in the distribution of hot halo gas, and the relationships between O VI and other highly ionized species including Si IV, C IV, and N V. This work is supported by NASA contract NAS5-32985.
Friedman Scott David
FUSE Science Team
Jenkins Edward B.
Kruk J. D.
Moos Warren H.
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