FUV intensities for the observed and simulated maps in Figure \[fig:fims\](a) and Figure \[fig:simul\](a), respectively. 194 stars selected as photon sources are marked in (a): black symbols correspond to the stars closer than 200 pc, and red symbols correspond to the stars located farther than 200 pc. The symbol size is proportional to the 1565 [Å]{} band flux of the TD-1 star catalog in log scale. \[fig:simul\]](f2b.eps "fig:"){width="7cm"}\

![image](f3a.eps){width="5.2cm"} ![image](f3b.eps){width="5.2cm"} ![image](f3c.eps){width="5.2cm"}\
![image](f3d.eps){width="5.2cm"} ![image](f3e.eps){width="5.2cm"} ![image](f3f.eps){width="5.2cm"}\

Simulation Model and Result
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As the observed FUV intensity generally follows the dust extinction level in Figure \[fig:fims\](a), with fluctuations which may be attributable to the local background UV radiation fields, most of the FUV diffuse emission in the OES region seems to originate from dust scattering of the radiation fields produced by nearby stars. Hence, it might be possible to obtain useful information regarding the distribution and scattering properties of dust from the observed FUV continuum map by comparing it with simulations based on theoretical predictions. We have performed Monte Carlo simulations, in which photons originating from bright stars are multiply scattered by assumed distributions of dust. We adopted the following Henyey-Greenstein scattering phase function $\Phi$($\theta$) [@hen41] for the dust scattering model, which is 