High-velocity OVI in and near the Milky Way

Details High-velocity OVI in and near the Milky Way High-velocity OVI in and near the Milky Way

2004-09-24

arxiv.org/abs/astro-ph/0409586v1

Astronomy and Astrophysics

Astrophysics

Contribution for "Extraplanar Gas" conference, held in Dwingeloo, June 2004

Scientific paper

The Far Ultraviolet Spectroscopic Explorer (FUSE) has observed over three hundred fifty sightlines to extragalactic targets. About one hundred fifty of these are of sufficient quality to measure OVI absorption in and near the Milky Way. High-velocity OVI absorption is detected in about 80% of the sightlines, with the detection rate going up for sightlines with higher signal-to-noise ratios. OVI is almost always seen in directions with previously known HI HVCs, including HVCs complex C, complex A, complex WD, the Magellanic Stream, and the Outer Arm. Studies of several sightlines through complex C suggest that the OVI absorption is produced in conductive interfaces between the cool HVC and a hotter surrounding medium, most likely a corona around the Milky Way. The OVI detections associated with the Magellanic Stream imply that this hot corona has a radius of at least 50 kpc. About half of the detections of high-velocity OVI are in directions where no high-velocity HI was previously known. Some of these are probably associated with the Magellanic Stream, others may represent Local Group gas. Still others often show up as a distinct wing on the low-velocity absorption; these may either represent an outflow from the Milky Way associated with the Galactic Fountain, they may be extragalactic HVCs, or they may be tracing a wind from the Galactic Center. Distance limits to the high-velocity OVI are scarce, but at least one of the clouds appear to be more distant than 4 kpc.

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