Background observations obtained with the Far Ultraviolet Spectroscopic Explorer ( FUSE ) toward l = 95 \fdg 4 , b = 36 \fdg 1 show O vi \lambda \lambda 1032,1038 in emission .
This sight line probes a region of stronger-than-average soft X-ray emission in the direction of high-velocity cloud Complex C above a part of the disk where H \alpha filaments rise into the halo .
The O vi intensities , 1600 \pm 300 photons s ^ { -1 } cm ^ { -2 } sr ^ { -1 } ( 1032 Å ) and 800 \pm 300 photons s ^ { -1 } cm ^ { -2 } sr ^ { -1 } ( 1038 Å ) , are the lowest detected in emission in the Milky Way to date .
A second sight line nearby ( l = 99 \fdg 3 , b = 43 \fdg 3 ) also shows O vi \lambda 1032 emission , but with too low a signal-to-noise ratio to obtain reliable measurements .
The measured intensities , velocities , and FWHMs of the O vi doublet and the C ii ^ { \ast } line at 1037 Å are consistent with a model in which the observed emission is produced in the Galactic halo by hot gas ejected by supernovae in the Perseus arm .
An association of the observed gas with Complex C appears unlikely .