types of structures, a thin shell surrounding the hot cavity and a thick dust layer as part of the OMCC, coexist in these sub-regions. In fact, when the simulation was carried out separately for the upper and lower parts of these sub-regions, their thicknesses were $\sim$100-140 pc for the upper parts and 10-30 pc for the lower parts for both of the sub-regions, in accordance with the environments of a thick dust region to the north and a thin shell to the south. In reality, the structure of the dust clouds would be more complex than we have assumed in the present study. However, we believe that our results provide an overall structure of the dust clouds toward the OES region.

With the new distance estimation for each of the sub-regions, we would like to compare the *E*(*B-V*) values derived from the distances of the dust layers with the observed *E*(*B-V*) values for the OES stars listed in the catalog of @fri92. While the derived *E*(*B-V*) values suffer from many error sources, as the present study modeled very simple dust layers and the observed *E*(*B-V*) values are based on the stellar models that involve uncertainties, we believe such a comparison 