The Cosmic Ultraviolet Background at the Galactic Poles
We have used archival GALEX data to separate the cosmic ultraviolet background at the Galactic Poles into two components: the dust scattered light and an offset. We have modeled the dust-scattered light using a single- scattering model finding 1 sigma limits of 0.54 -- 0.71 for the albedo (a) and 0.74 -- 0.83 for the phase function asymmetry factor (g) at 1530 {\AA} and 0.66 -- 0.73 for a and 0.71 -- 0.77 for g at 2360 {\AA}, that is, the grains are moderately reflective and highly forward-scattering. The offsets are 277 -- 284 photon units at 1530 {\AA} and 513 -- 520 photon units at 2360 {\AA}. We have estimated other Galactic and extragalactic contributors to the offset finding that 161 +- 18 photon units is unaccounted for at 1530 {\AA} and 335 +- 38 at 2360 {\AA}. The offsets are constant over these regions with variances of 20 -- 30 photon units.