We intend to search for diffuse intergalactic dust emission in Hickson compact groups (HCG's). Evidence has surfaced in the last few years for a diffuse component in loose groups which are regarded as the precursors of compact groups (CG's). HI, optical and X-ray data all show evidence for a diffuse component in the intragroup medium (IGM) of CG's. The X-ray observations find evidence for both solar and primordial abundance IGM emission in different CG's. The latter emission would likely originate from stripping during the frequent galaxy-galaxy encounters in the CG's. We would like to target two CG's with the highest likelihood to show diffuse IGM dust emission. They are spiral rich, FIR bright and, in the case of HCG 92, show evidence for solar abundance in the hot intragroup gas. Our calculations suggest that such an intragroup dust component can survive (and is detectable) in groups with diffuse hot gas especially if they are as dynamically young as the models suggest. It will be very interesting to compare the properties of intragroup dust if detected with intracluster dust emission that we expect will be detected by ISO. The observations will also help to resolve the ambiguity over which galaxies in these groups are FIR emitters. The ambiguity resulted from the resolution limitations of IRAS. This aspect is not discussed further in the proposal.