The IOTA interferometer has been in scheduled operation since 1995 with two 0.45 m telescopes, and baselines of up to 38 m; a third telescope will be installed in 1998 and three-beam combination will be implemented in 1999. We currently have three major detection systems, built around a CCD, a NICMOS3, and the FLUOR fiber beam combiner. A piezo- driven rapid scan delay is also available. Our experience in using these systems is reviewed here, and the corresponding magnitude limits of fringe measurements in the V, R, I, J, H, K bands are discussed. Recent result from these new detector systems include measurements of stellar diameters and temperatures, stellar surface features, and circumstellar dust emission.