  The FIRAS instrument on the COBE satellite has conducted an unbiased survey
of the far-infrared emission from our Galaxy. The first results of this survey
were reported by Wright et al. (1991). We report the results of new analyses of
this spectral survey, which includes emission lines from 158 um C+, 122 um and
205 um N+, 370 um and 609 um C, and CO J=2-1 through 5-4. We report the
morphological distribution along the galactic plane (b=0) of the spectral line
emission, and the high galactic latitude intensities of the C+ and 205 um N+
emission. The high galactic latitude intensity cosecant of the 158 um fine
structure transition from C+ is presented, and C+ is seen to decrease more
rapidly than the far infrared intensity with increasing galactic latitude. C+
and H I emission are closely correlated with a C+ cooling rate of (2.65 +/-
0.15)x10^{-26} erg/s/H-atom. We conclude that this emission arises almost
entirely from the Cold Neutral Medium. The high galactic latitude intensity of
the 205 um fine structure transition from N+ arises entirely from the Warm
Ionized Medium, and its cosecant is presented. We estimate the total ionizing
photon rate in the Galaxy to be 3.5x10^{53} ionizing photons per second, based
on the 205 um N+ transition.
