Far‐infrared fine structure and its interstellar counterparts

Mosaics at 60 μm and 100 μm have been constructed of the 60°×60° area covering the Galactic center, bulge, molecular ring, and nearby clouds of emitting dust. We examine the relationship between various tracers of the interstellar medium and the fine‐scale structure that is evident in these mosaics. We pay special attention to the nearby Ophiucus cloud complex, a spectacular showcase for interactions between hot stars and dense interstellar matter. Here, the CO emission correlates well with much of the warm dust emission, whereas the Hα and FIR emission appear mostly uncorrelated. The warmest FIR colors are associated with the positions of young hot stars. Closer to the Galactic plane, the FIR fine structure is more likely tracing enhancements of warm dust in the more distant molecular ring and central bulge.