Computer Science
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..281..155s&link_type=abstract
The IGM/Galaxy Connection: The Distribution of Baryons at z=0, ASSL Conference Proceedings Vol. 281. Edited by Jessica L. Rosenb
Computer Science
Scientific paper
We have completed our large FUSE survey of high velocity OVI absorption along ~100 complete sight lines through the Galactic halo. The high velocity OVI traces tidal interactions with the Magellanic Clouds, accretion of gas, outflowing material from the Galactic disk, warm/hot gas interactions in a highly extended Galactic corona, and intergalactic gas in the Local Group. Approximately 60% of the sky (and perhaps as much as 85%) is covered by high velocity hot H+ associated with the high velocity OVI. Some of the OVI may be produced at the boundaries between warm clouds and a hot, highly-extended Galactic corona or Local Group medium. A hot Galactic corona or Local Group medium and the prevalence of high velocity OVI are expected in various galaxy formation scenarios. Additional spectroscopic data in the coming years will help to determine the ionization properties of the high velocity clouds and discriminate between the multiple types of high velocity OVI features found in this study.
Jenkins Edward B.
Meade Marilyn
Richter Philipp
Savage Blair. D.
Sembach Kenneth Russell
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