The [ITAL]Far Ultraviolet Spectroscopic Explorer[/ITAL] Detection of Galactic O [CSC]vi[/CSC] Emission in the Halo above the Perseus Arm | Zendy

B. Otte | Zendy; W. V. Dixon | Zendy; Ravi Sankrit | Zendy

Open Access

The [ITAL]Far Ultraviolet Spectroscopic Explorer[/ITAL] Detection of Galactic O [CSC]vi[/CSC] Emission in the Halo above the Perseus Arm

Author(s) -

B. Otte,

W. V. Dixon,

Ravi Sankrit

Publication year - 2003

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/374731

Subject(s) - physics , astrophysics , milky way , halo , emission spectrum , ultraviolet , line (geometry) , supernova , galactic halo , line of sight , galactic corona , astronomy , spectral line , galaxy , optics , geometry , mathematics

Background observations obtained with the Far Ultraviolet SpectroscopicExplorer (FUSE) toward l=95.4, b=36.1 show OVI 1032,1038 in emission. Thissight line probes a region of stronger-than-average soft X-ray emission in thedirection of high-velocity cloud Complex C above a part of the disk whereHalpha filaments rise into the halo. The OVI intensities, 1600+/-300ph/s/cm^2/sr (1032A) and 800+/-300 ph/s/cm^2/sr (1038A), are the lowestdetected 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 asignal-to-noise ratio to obtain reliable measurements. The measuredintensities, velocities, and FWHMs of the OVI doublet and the CII* line at1037A are consistent with a model in which the observed emission is produced inthe Galactic halo by hot gas ejected by supernovae in the Perseus arm. Anassociation of the observed gas with Complex C appears unlikely.Comment: accepted for publication in ApJL, 11 pages including 3 figure

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