CII Diffuse Emission Observed by IRTS
CII Diffuse Emission Observed by IRTS
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IRTS 观测到的 CII 漫发射
DOI：
10.1093/pasj/48.6.l127
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发表时间：
1996
影响因子：
2.3
通讯作者：
K. Okumura
中科院分区：
文献类型：
--
作者：
H. Shibai;H. Okuda;T. Nakagawa;S. Makiuti;H. Matsuhara;N. Hiromoto;K. Okumura
用高灵敏度、高分辨率的远红外测线仪(膜)观测到了CII158μm谱线发射和155μm远红外连续谱发射。观测是沿着L=50°和230°的银面上的一个大圆进行的。在它们的强度分布中发现了两个成分。第一个分量集中在银河系平面上。它在L=50°平面上很明显，但在230°时很微弱。第二个分量在银河系纬度上延伸至少20°，在银河系平面的两个相交部分具有几乎相同的强度。因此，第一个分量可以归因于星系盘的发射，第二个分量可以归因于本地星际气体的发射。第二个分量的[CII]线的强度分布与HI 21 cm积分强度的分布相似。这一事实表明，局地[CII]发射分量出现在HI 21 cm放气线上。根据CII线光度与氢柱密度的比值，HI气体的星际冷却速率为(5.6±2.6)×10−2 7erg S−1/H原子，对应于压力为几百cm−3K的冷中性气体。
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) × 10−27erg s−1/H-atom, corresponding to the cold neutral gas whose pressure is a few hundred cm−3K.