FUSE Detection of Galactic OVI Emission in the Halo above the Perseus Arm

Details FUSE Detection of Galactic OVI Emission in the Halo above the Perseus Arm FUSE Detection of Galactic OVI Emission in the Halo above the Perseus Arm

2003-02-12

arxiv.org/abs/astro-ph/0302251v1

Astrophys.J. 586 (2003) L53-L56

Astronomy and Astrophysics

Astrophysics

accepted for publication in ApJL, 11 pages including 3 figures

Scientific paper

10.1086/374731

Background observations obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) toward l=95.4, b=36.1 show OVI 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 Halpha filaments rise into the halo. The OVI intensities, 1600+/-300 ph/s/cm^2/sr (1032A) and 800+/-300 ph/s/cm^2/sr (1038A), are the lowest detected in emission in the Milky Way to date. A second sight line nearby (l=99.3, b=43.3) also shows OVI 1032 emission, but with too low a signal-to-noise ratio to obtain reliable measurements. The measured intensities, velocities, and FWHMs of the OVI doublet and the CII* line at 1037A 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.

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