Abstract
The CII 158 μm line emission and the far-infrared continuum emission at 155 μm were observed by the Far-Infrared Line Mapper (FILM) aboard the Infrared Telescope in Space (IRTS) with its high sensitivity and resolution. The observation was made along a great circle crossing the galactic plane at l = 50° and 230°. Two components were found in their intensity distributions. The first component concentrates on the galactic plane. It is prominent on the plane at l = 50°, but is very faint at 230°. The second component extends over at least 20° in galactic latitude, and has nearly the same intensity at both crossing parts of the galactic plane. Therefore, the first one can be ascribed to emission from the galactic disk, and the second component to emission from the local interstellar gas. The intensity distribution of the [CII] line of the second component is similar to that of the HI 21 cm integrated intensity. This fact suggests that the local [CII] emission component arises in the HI 21 cm line emitting gas. From the ratio of the CII line luminosity to the hydrogen column density, the interstellar cooling rate of the HI gas is (5.6 ± 2.6) × 10−27 erg s−1/H-atom, corresponding to the cold neutral gas whose pressure is a few hundred cm−3 K.
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