Comparison of Diffuse Infrared and Far-Ultraviolet emission in the Large
  Magellanic Cloud: The Data
  Dust scattering is the main source of diffuse emission in the far-ultraviolet
(FUV). For several locations in the Large Magellanic Cloud (LMC), Far
Ultraviolet Spectroscopic Explorer (FUSE) satellite has observed diffuse
radiation in the FUV with intensities ranging from 1000 - 3 X 10^5 photon units
and diffuse fraction between 5% - 20% at 1100 {\deg}A. Here, we compare the FUV
diffuse emission with the mid-infrared (MIR) and far-infrared (FIR) diffuse
emission observed by the Spitzer Space Telescope and the AKARI satellite for
the same locations. The intensity ratios in the different MIR and FIR bands for
each of the locations will enable us to determine the type of dust contributing
to the diffuse emission as well as to derive a more accurate 3D distribution of
stars and dust in the region, which in turn may be used to model the observed
scattering in the FUV. In this work we present the infrared (IR) data for two
different regions in LMC, namely N11 and 30 Doradus. We also present the FUV~IR
correlation for different infrared bands.
