of two-photon emissions. Therefore, we have not removed the two-photon continuum emission, which may make the two arcs appear more prominently, and will instead discuss its contribution to the map. The final image was obtained with 1$^\circ$ $\times$ 1$^\circ$ pixel bins and is shown in Figure \[fig:fims\](a), overplotted with dust contours.

When the new map of Figure \[fig:fims\](a) is compared with the previous diffuse FUV map, Figure 2(a) of @jo11, which includes the contributions of the ion lines as well as the H$_2$ fluorescent emission, we can see that overall morphology did not change much. The most significant change due to the exclusion of the ion lines is seen only in the northeastern region of the map near the left boundary above $\delta$ = 0$^\circ$, where the scattered photons of the two bright B-type stars with strong P Cygni profiles, HD 31237 and HD 30836 located at ($\alpha$, $\delta$) $\sim$ (73$^\circ$.6, 2$^\circ$.4) and (72$^\circ$.8, 5$^\circ$.6), respectively, are responsible for the enhanced emissions. The H$_2$ fluorescent emission varied significantly according to the regions as can be seen in Figure 2(b) of @jo11 while it is $\sim$17$\%$ on average for the whole OES region, as can be estimated from the spectrum of 