correspond to the regions of light blue to green in the western part of the OMCC. As noted in @jo11, the western part of the Complex shows lower FUV intensity than its eastern counterpart because it contains fewer stars as interstellar radiation sources. Hence, we see a linear relationship between FUV intensity and dust extinction in the blue regions of Figure \[fig:fims\](a) where dust extinction is small while the scattered data points in Figure \[fig:fims\](b) seem to be related to the fluctuations in the background UV radiation fields.

![(a) FUV continuum map obtained from dust scattering simulation for a single dust slab, and (b) a pixel-to-pixel scatter plot of the 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. \[fig:simul\]](f2a.eps "fig:"){width="7.3cm"}\
![(a) FUV continuum map obtained from dust scattering simulation for a single dust slab, and (b) a pixel-to-pixel scatter plot of the 