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Observations of O VI Emission from the Diffuse Interstellar Medium
We report the first Far-Ultraviolet Spectroscopic Explorer measurementsof diffuse O VI (λλ1032, 1038) emission from the generaldiffuse interstellar medium outside of supernova remnants orsuperbubbles. We observed a 30''×30'' regionof the sky centered at l=315.0d and b=-41.3d. From the observedintensities (2930+/-290 [random]+/-410 [systematic] and 1790+/-260[random]+/-250 [systematic] photons cm-2 s-1sr-1 in λλ1032 and 1038, respectively), derivedequations, and assumptions about the source location, we calculate theintrinsic intensity, electron density, thermal pressure, and emittingdepth. The intensities are too large for the emission to originatesolely in the Local Bubble. Thus, we conclude that the Galactic thickdisk and lower halo also contribute. High-velocity clouds are ruled outbecause there are none near the pointing direction. The calculatedemitting depth is small, indicating that the O VI-bearing gas fills asmall volume. The observations can also be used to estimate the coolingrate of the hot interstellar medium and to constrain models. The dataalso yield the first intensity measurement of the C II 3s2S1/2-2p 2P3/2 emission lineat 1037 Å and place upper limits on the intensities of ultravioletline emission from C I, C III, Si II, S III, S IV, S VI, and Fe III.
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