FAR-INFRARED SPECTRAL OBSERVATIONS OF THE GALAXY BY COBE

We derive Galactic continuum spectra from 5-96 cm(-1) from COBE/FIRAS observations. The spectra are dominated by warm dust emission, which may be fitted with a single temperature in the range 16-21 K (for nu(2) emissivity) along each line of sight. Dust heated by the attenuated radiation field in molecular clouds gives rise to intermediate-temperature (10-14 K) emission in the inner Galaxy only. A widespread, very cold component (4-7 K) with optical depth that is spatially correlated with the warm component is also detected. The cold component is unlikely to be due to very cold dust shielded from starlight because it is present at high latitude. We consider hypotheses that the cold component is due to enhanced submillimeter emissivity of the dust that gives rise to the warm component, or that it may be due to very small, large, or fractal particles. Lack of substantial power above the emission from warm dust places strong constraints on the amount of cold gas in the Galaxy. The microwave sky brightness due to interstellar dust is dominated by the cold component, and its angular variation could limit our ability to discern primordial fluctuations in the cosmic microwave background radiation.