Galactic light [@seo11], the optical properties of the dust grains, generally characterized by the albedo and the phase function asymmetry factor *g* $\equiv$ $<\cos\theta>$, can be inferred from the observations of the diffuse Galactic light. The observations can also be compared with model calculations. For example, @dra03 estimated the albedo and *g*-factor for the carbonaceous-silicate grains, and obtained $\sim$0.40 and $\sim$0.65 for the albedo and the *g*-factor at $\lambda$ $\sim$ 1600 [Å]{}, respectively. While the values of the albedo and g-factor are clearly dependent on the models of dust grains, accurate photometry and modeling of dust clouds are also required for reliable estimations of these optical properties from observations. Until now, there have been numerous studies in this line of research from the early 70’s, especially at far-ultraviolet (FUV) and near-ultraviolet (NUV) wavelengths [@wit73; @wit78; @lil76; @mor78; @mor82; @mor80; @ona84; @wit92; @wit97; @gor94; @cal95]. For example, the observations made from the *Voyager 2* spacecraft have been used for the wavelengths shorter than 1200 [Å]{} [@wit93; @mur93; @bur02; @sha04; @sha06; @suj05; @suj07]. A comparative review of past work can be found in @gor04. Recently, *GALEX* observations provided diffuse UV background images with high spatial resolution, which have been used for the 