A Hole in the Galaxy's Emissive O VI Coverage

Details A Hole in the Galaxy's Emissive O VI Coverage A Hole in the Galaxy's Emissive O VI Coverage

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.1603m&link_type=abstract

American Astronomical Society Meeting 208, #16.03; Bulletin of the American Astronomical Society, Vol. 38, p.97

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Scientific paper

We report observations of O VI resonance line emission (1032, 1038 Angstroms) along the sight line to NGC 1068 (l = 172.1, b=-51.9), made using the Far Ultraviolet Spectroscopic Explorer's (FUSE) low resolution aperture (LWRS). The observations place tight upper limits on the O VI emission originating in our galaxy's diffuse interstellar medium as well as tight upper limits on the emission originating in NGC1068's extended disk. The Milky Way's intensities in the 1032 and 1038 Angstrom emission lines are 170 ± 300 and -70 ± 280 photons cm-2 s-1 sr-1 respectively. These values are an order of magnitude less than those observed on other unobscured, high latitude sight lines, indicating a hole in the distribution of emissive interstellar O VI ions. Nonetheless, extensive O VI column density surveys have found large O VI column densities on every sampled extragalactic line of sight, including a line of sight only 2 arcminutes from our pointing direction. From the \frac{IO VI}{NO VI} ratio, we find that the gas in this direction is either extremely rarefied (ne < 0.001 cm-3) or much cooler than its collisional ionizational equilibrium temperature. It's character must differ from the emissive O VI seen toward other high latitude directions.We also made the first search for O VI emission from the disk of a Seyfert galaxy, using NGC 1068. The intensities in the redshifted O VI emission lines (1036 and 1042 Angstroms) are 10 ± 290 and 510 ± 320 photons cm-2 s-1 sr-1, respectively. These are surprisingly tight upper limits for a galaxy known to have starburst activity in its disk and an AGN in its center.

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