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A complete survey of the central molecular zone in NH3

机译：NH3中心分子区的完整调查

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摘要

We present a map of the major part of the central molecular zone (CMZ) of simultaneous observations in the NH3 (J, K) = (1,1) and (2,2) lines using the Kagoshima 6 m telescope. The mapped area is -1.degrees 000 >= I <= 10625 and -0.degrees 375 <=< b <= 0.degrees 0250. The kinetic temperatures derived from the (2,2) to (],I) intensity ratios are 20-80 K, or exceed 80 K. The gases corresponding to temperatures of 20-80 K and >= 80 K contain 75% and 25% of the total NH3 flux, respectively. These temperatures indicate that the dense molecular gas in the CMZ is dominated by gas that is warmer than the majority of the dust present there. A comparison of our observations with a CO survey by Sawada et al. (200 1, ApJS, 136, 189) shows that the NH3 emitting region is surrounded by a high-pressure region on the longitude-velocity (1-v) plane. Although NH3 emission traces dense gas, it does not extend over a high-pressure region. Therefore, the high-pressure region is less dense and has to be hotter. This indicates that the molecular-cloud complex in the Galactic center region has a "core" of dense and warm clouds that are traced by the NH3 emission, and an "envelope" of less-dense and hotter gas clouds. Besides heating by ambipolar diffusion, the hot plasma gas emitting the X-ray emission may heat the hot "envelope".
机译：我们提供了使用鹿儿岛6 m望远镜同时观测NH3（J，K）=（1,1）和（2,2）线的中央分子区（CMZ）的主要部分的地图。映射的区域为-1度000> = I <= 10625和-0度375 <= = 80 K温度的气体分别占总NH3通量的75％和25％。这些温度表明，CMZ中的致密分子气体主要是比那里的大多数粉尘更热的气体。我们的观察结果与Sawada等人的CO调查结果的比较。 （200 1，ApJS，136，189）显示，NH3发射区域在经度-速度（1-v）平面上被高压区域包围。尽管NH3的排放物跟踪到的是高浓度气体，但它不会在高压区域延伸。因此，高压区域密度较小并且必须更热。这表明，银河系中心区域的分子云复合体具有由NH3排放所追踪的密集而温暖的云的“核心”，以及密度较小而较热的气体云的“包络”。除了通过双极扩散进行加热之外，发射X射线发射的热等离子体气体还可以加热热的“信封”。

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