O VI Emission from the Hot Diffuse Interstellar Medium

Details O VI Emission from the Hot Diffuse Interstellar Medium O VI Emission from the Hot Diffuse Interstellar Medium

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000head....5.4413s&link_type=abstract

American Astronomical Society, HEAD Meeting #5, #44.13; Bulletin of the American Astronomical Society, Vol. 32, p.1653

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Scientific paper

We report Far Ultraviolet Spectroscopic Explorer (FUSE) measurements of diffuse O VI (λ λ 1032,1038) emission from the southern sky toward l = 315.0o and b = -41.3o. There are no known point sources, supernova remnants, or superbubbles in this directions and the soft X-ray maps indicate that this region is representative of the southern sky. The expected sources for the observed emission are the Local Bubble and gaseous Galactic halo, though in the latter case, the flux may be attenuated by roughly 50%. The O VI surface brightnesses in the 1032 and 1038 Å components from this direction are 2900 +/- 270 and 1900 +/- 260 photons cm-2 sec-1 sr-1, respectively. We derive the electron density and thermal pressure of the emitting plasma from an isothermal model and estimates of the O VI column density for the Local Bubble and Galactic halo. We conclude that the observed flux is too bright to have originated entirely in the Local Bubble, hence the Galactic halo must have produced most of the flux. We also measured the C II* surface brightness and placed upper limits on the surface brightnesses of ultraviolet emission lines of C I, C III, Si II, S III, S IV, S I, and Fe II.

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