Far-IR Spectroscopic Survey of the Galactic Plane by the Balloon IR Telescope

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Strong [CII] emission has been ubiquitously detected all over the region between 1 = 30ﾟ and 51ﾟ, and the intensity distribution is rather smoot extended far from discrete luminous HII regions. Latitudinal and longitudinal pr the [CII] intensity distribution are quite similar to those of ^<12>CO(J = 1-0) resemble those of IRAS flux, while they are completely different from those of The diffuse [CII] emission probably comes from the C^+ regions (a part o photodissociation regions), which are illuminated by the general interstellar UV field and form as mantles of giant molecular clouds traced by ^<12>CO. The ext density ionized gas may also contribute to the diffuse [CII] emission. The mass resions is at least 40% of that of CO molecular gas. The total energy of the [emitted from the inner Galactic disk amounts to 2.8 x 10^7 times of the solar 1 which corresponds to 0.36% of the total far-infrared luminosity of the same regi