dust distribution, and the result of our simulations should be regarded as a representative one, indicating the effective distance and thickness. In the present simulation, the *E*(*B-V*) values of the SFD dust map for given sightlines were converted into the optical depths at 1565 [Å]{}, which was regarded as a representative FUV wavelength of the FIMS observation, and then assigned to the grid points with equal distribution for an assumed cloud thickness. As we learned that most of the dust is located within $\sim$400 pc from the Sun in the direction toward the OES (@ver10; Vergely 2011 private communication), we took a single dust slab and placed it within 400 pc with the whole dust extinction from the SFD map distributed equally among the grids for an assumed thickness. We will further consider possible improvements to our model in the Discussion section.

Along with the distance and thickness of the dust slab, the albedo and phase function asymmetry factor, which are the optical parameters related to the scattering properties of dust, were varied. The ranges of simulation parameters were as follows: the distance to the front face varied from 10 pc to 200 pc with 10 pc steps, the thickness 