plot of the FUV intensities taken from the observed and simulated maps in Figure \[fig:fims\](a) and Figure \[fig:simul2\](a), respectively.\[fig:simul2\]](f4b.eps "fig:"){width="7cm"}\

The best fitting values for the 9 sub-regions are shown in Table \[tbl:simul2\], and the resulting mosaic map constructed with these fitting parameters is depicted in Figure \[fig:simul2\](a), together with the pixel-to-pixel scatter plot of the FUV intensities in Figure \[fig:simul2\](b). As Figure \[fig:simul2\](b) shows, the simulation result is much improved now when compared with the previous result shown in Figure \[fig:simul\](b), with the new reduced chi-square value of $\chi^2$ $\sim$ 3.19. The most remarkable change is seen in the sub-region 7, of which the intensity increased. Noting that the thickness increased dramatically for this region, we believe the reason for the intensity increase in sub-region 7 is that more stellar sources reside in the cloud now and can contribute to the scattered continuum. We also note that the contribution from the two-photon effect, estimated as a difference of the FUV intensity between Figure \[fig:fims\](a) and Figure \[fig:simul2\](a), has decreased to $\sim$15-30$\%$, by $\sim$10$\%$ from the previous result.

While the best fitting parameters shown in Table \[tbl:simul2\] may still not be exact, they seem to provide meaningful insights into the 