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We present results of our survey observations of the [C II] 158 µm line emission from the Galactic plane using the Balloon-borne Infrared Carbon Explorer (BICE). Our survey covers a wide area (350 • ∼ < l ∼ < 25 • , |b| ∼ < 3 • ) with a spatial resolution of 15 ′ . We employed a new observing method called the "fast spectral scanning" to make large-scale observations efficiently.Strong [C II] line emission was detected from almost all areas we observed. In the general Galactic plane, the spatial distribution of the [C II] line emission correlates very well with that of far-infrared continuum emission, but diffuse components are more prominent in the [C II] line emission; the I [CII] /I FIR ratio is ∼ 0.6 % for diffuse components but is ∼ 0.2 % for compact sources such as active star-forming regions. In the Galactic center region, on the other hand, the distribution of the [C II] line emission is quite different from that of the far-infrared continuum emission, and the I [CII] /I FIR ratio is systematically lower there.The FWHM velocity resolution of our instrument is 175 km s −1 , but we determined the central velocity of the line at each observed point very precisely with statistical

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We have made one-dimensional raster scan observations of the Oph and Sco star-forming regions with two spectrometers (SWS and LWS) on board the ISO.

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