for a year and a half. With its large image fields of view (S-band: 4$^\circ$.0$\times$4’.6, L-band: 7$^\circ$.5$\times$4’.3) and moderate spectral ($\lambda/\Delta\lambda$ $\sim$ 550) and angular ($\sim$5’) resolutions, the instrument is optimized for the observation of diffuse emissions [@ede06a; @ede06b]. Though the OES region was observed in both the S- and L-band, we analyzed only the L-band data for the present study since the S-band data were strongly contaminated by geocoronal emission lines. Bright point sources were removed from the map: a total of 210 stars in the TD-1 catalog with 1565 [Å]{} band fluxes of above 10$^{-12}$ ergs [Å]{}$^{-1}$ s$^{-1}$ cm$^{-2}$ were removed, and the remaining bright pixels, not corresponding to the stars listed in the TD-1 catalog, were also removed. More information on the data reduction procedures can be found in @jo11.

While stellar UV radiation scattered by interstellar dust grains is generally known to be the most dominant source of diffuse FUV emission, there are other contributors such as atomic line emissions, extragalactic background, H$_2$ fluorescence, and two-photon continuum emissions. Hence, it is necessary to eliminate these extra contributions in order to obtain more reliable results for the effect of dust scattering. For example, the atomic lines were 