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In order to examine their relation to the host galaxy, the extraplanar dustof six nearby galaxies are modeled, employing a three dimensional Monte Carloradiative transfer code. The targets are from the highly-inclined galaxies thatshow dust-scattered ultraviolet halos, and the archival Galaxy EvolutionExplorer FUV band images were fitted with the model. The observed images are ingeneral well reproduced by two dust layers and one light-source layer, whosevertical and radial distributions have exponential profiles. We obtainedseveral important physical parameters, such as star formation rate (SFR_UV),face-on optical depth, and scale-heights. Three galaxies (NGC 891, NGC 3628,and UGC 11794) show clear evidence for the existence of extraplanar dust layer.However, it is found that the rest three targets (IC 5249, NGC 24, and NGC4173) do not necessarily need a thick dust disk to model the ultraviolet (UV)halo, because its contribution is too small and the UV halo may be caused bythe wing part of the GALEX point spread function. This indicates that thegalaxy samples reported to have UV halos may be contaminated by galaxies withnegligible extraplanar (halo) dust. The galaxies showing evidence of theextraplanar dust layer fall within a narrow range on the scatter plots betweenphysical parameters such as SFR_UV and extraplanar dust mass. Severalmechanisms possible to produce the extraplanar dust are discussed. We alsofound a hint that the extraplanar dust scale-height might not be much differentfrom the polycyclic aromatic hydrocarbon emission characteristic height.

Ultraviolet Radiative Transfer Modeling of Nearby Galaxies with Extraplanar Dusts