removed as follows. We took only the 1420 [Å]{}-1630 [Å]{} portion from the L-band spectrum to exclude the bright airglow lines at 1356 [Å]{} and 1641 [Å]{} as well as other atomic/ionic lines such as \] 1407 [Å]{}, 1640 [Å]{}, 1657 [Å]{}, and 1671 [Å]{}, as identified previously in Table 1 of @jo11. The remaining spectrum still included the \* and lines centered at 1533 [Å]{} and 1549 [Å]{}, respectively, which were removed by excluding the spectral range from 1525 [Å]{} to 1560 [Å]{}. We have constructed a diffuse FUV map with the remaining portion of the spectrum.

The extragalactic diffuse FUV background is known to be more or less uniform over the celestial sphere with $\sim$300 Continuum Units (CU), and is expected to be even more so at high galactic latitudes [@bow91]. Noting that OES is located at high galactic latitudes, we have subtracted 300 CU from the original diffuse emission map. The contribution of H$_2$ fluorescent emission was subtracted in the following way using the map of Figure 2(b) in @jo11. We first converted the original H$_2$ map, which was constructed from the 1608 [Å]{} line intensity, to a map of total H$_2$ emission for the whole wavelength 