The SiO outflow from IRAS 17233-3606 at high resolution
The SiO outflow from IRAS 17233-3606 at high resolution
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DOI：
10.1051/0004-6361/201424781
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发表时间：
2014-12
影响因子：
6.5
通讯作者：
P. Klaassen;K. Johnston;S. Leurini;L. A. L. Observatory-L.-A.-L.-Observatory-143706407;UK Astronomy Technology Centre;M. F. Astronomy;U. Leeds;M. F. Radioastronomie;C. D. Astrofisica;Unam
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文献类型：
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作者：
P. Klaassen;K. Johnston;S. Leurini;L. A. L. Observatory-L.-A.-L.-Observatory-143706407;UK Astronomy Technology Centre;M. F. Astronomy;U. Leeds;M. F. Radioastronomie;C. D. Astrofisica;Unam
背景：喷流和流出物是整个质谱中恒星形成的关键成分。在聚集区域，了解电源和流出组件构成了一个重大问题。目标：我们的目标是了解在形成大质量恒星的过程中星团流出的动态。方法：我们使用新的 VLA 观测结果对大质量恒星形成区域 IRAS 17233-3606 中的分子气体（SiO、CS、OCS 和 H2CO）进行观测，该区域包含许多 HII 区域。我们将这些观察结果与之前发布的该来源的分子数据进行比较，以便全面了解流出动态。结果：我们发现，与 HII 区域的大小相比，各种物种的动态可以通过单个大规模 (~0.15 pc) 流出来解释，蓝色和红色流出成分的不同形态可以根据周围包络的形态来解释。我们进一步发现，OCS 和 H2CO 中看到的速度梯度方向表明，在大规模外流底部附近的 HII 区域周围的温暖气体中存在旋转和外流运动的组合。结论。我们的结果表明，在该区域内形成的巨大原恒星似乎促成了大规模的单一流出。当流出物与周围环境相互作用时，许多不同的物种都会追踪到这种单一的大规模流出物。在小尺度上，似乎有多种机制对动态有贡献，这些机制可能是小规模流出或旋转与大规模流出动态的组合。
Context: Jets and outflows are key ingredients in the formation of stars across the mass spectrum. In clustered regions, understanding powering sources and outflow components poses a significant problem. Aims: We aim to understand the dynamics in the outflow(s) from a cluster in the process of forming massive stars. Methods: We use new VLA observations of the molecular gas (SiO, CS, OCS, and H2CO ) in the massive star forming region IRAS 17233-3606 which contains a number of HII regions. We compare these observations to previously published molecular data for this source in order to get a holistic view of the outflow dynamics. Results: We find that the dynamics of the various species can be explained by a single large scale (~0.15 pc) outflow when compared to the sizes of the HII regions, with the different morphologies of the blue and red outflow components explained with respect to the morphology of the surrounding envelope. We further find that the direction of the velocity gradients seen in OCS and H2CO are suggestive of a combination of rotation and outflow motions in the warm gas surrounding the HII regions near the base of the large scale outflow. Conclusions. Our results show that the massive protostars forming within this region appear to be contributing to a single outflow on large scales. This single large scale outflow is traced by a number of different species as the outflow interacts with its surroundings. On the small scales, there appear to be multiple mechanisms contributing to the dynamics which could be a combination of either a small scale outflow or rotation with the dynamics of the large scale outflow.