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We present a new method to evaluate the dust extinction (AV) along the lineof sight using the InfraRed Survey Facility (IRSF) near-infrared (NIR) data ofthe Large Magellanic Cloud (LMC) HI ridge region. In our method, we estimate anAV value for each star from the NIR color excess and sort them from bluer toredder in each line of sight. Using the percentile values of the sorted AV, wenewly construct the three-dimensional AV map. We compare the resultant AV mapwith the total hydrogen column density N(H) traced by velocity-resolved HI andCO observations. In the LMC HI ridge region, Fukui et al. (2017, PASJ, 69, L5)find two velocity components and an intermediate velocity one bridging them.Comparing our three-dimensional AV maps with N(H) maps at the differentvelocities, we find that the dust geometry is consistent with the scenario ofthe on-going gas collision between the two velocities as suggested in theprevious study. In addition, we find difference by a factor of 2 in AV/N(H)between the two velocity components, which suggests that inflow gas from theSmall Magellanic Clouds (SMC) is mixed in this region. As a whole, our resultssupport the triggered star formation in 30 Doradus due to the large-scale gascollision caused by tidal interaction between the LMC and the SMC.

Three-dimensional dust geometry of the LMC HI ridge region as revealed by the IRSF/SIRIUS survey