  We derive Galactic continuum spectra from 5-96/cm from COBE/FIRAS
observations. The spectra are dominated by warm dust emission, which may be fit
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.
