围绕大质量（原）星的候选旋转环
Candidate Rotating Toroids around High-Mass (Proto)Stars
摘要：
使用OVRO、Nobeyama和IRAM毫米阵列，我们在三个大质量（原）恒星形成区：G16.59-0.05、G23.01-0.41和G28.87+0.07中搜索了“盘”流出系统。这些是从与OH和H2O脉泽发射相关的NH3核心样本中选择的，并且没有或非常微弱的连续发射。我们对分子线（包括CH 3CN的旋转跃迁和3 mm尘埃连续发射）的成像显示，这些是紧凑、大质量和热的分子核（HMC），这可能是UCHII区出现之前的高质量恒星形成场所。所有这三个来源都与CO和/或HCO+ J=1- 0线成像的分子流出有关。此外，在G23.01和G28.87 HMCs的最内侧的致密区域的速度梯度为10 - 100公里/秒/秒的pc被确定沿大致垂直于相应的流出轴的方向。所有的结果表明，这些核心可能是围绕流出轴旋转，虽然旋转的重力平衡的HMC的贡献似乎是可以忽略不计的。我们的分析表明，由于湍流压力的支持，3个HMC接近维里平衡。与其他类似的物体相比，旋转环已经确定到目前为止，在我们的情况下，旋转似乎是不太突出，这可以解释为不利的投影，大的距离，有限的角分辨率与当前的干涉仪的综合效应。
英文摘要：
Using the OVRO, Nobeyama, and IRAM mm-arrays, we searched for ``disk''-outflow systems in three high-mass (proto)star forming regions: G16.59-0.05, G23.01-0.41, and G28.87+0.07. These were selected from a sample of NH3 cores associated with OH and H2O maser emission and with no or very faint continuum emission. Our imaging of molecular line (including rotational transitions of CH3CN and 3mm dust continuum emission revealed that these are compact, massive, and hot molecular cores (HMCs), that is likely sites of high-mass star formation prior to the appearance of UCHII regions. All three sources turn out to be associated with molecular outflows from CO and/or HCO+ J=1--0 line imaging. In addition, velocity gradients of 10 -- 100 km/s per pc in the innermost densest regions of the G23.01 and G28.87 HMCs are identified along directions roughly perpendicular to the axes of the corresponding outflows. All the results suggest that these cores might be rotating about the outflow axis, although the contribution of rotation to gravitational equilibrium of the HMCs appears to be negligible. Our analysis indicates that the 3 HMCs are close to virial equilibrium due to turbulent pressure support. Comparison with other similar objects where rotating toroids have been identified so far shows that in our case rotation appears to be much less prominent; this can be explained by the combined effect of unfavorable projection, large distance, and limited angular resolution with the current interferometers.
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