Volume 575, March 2015
|Number of page(s)||10|
|Section||Interstellar and circumstellar matter|
|Published online||23 February 2015|
The SiO outflow from IRAS 17233-3606 at high resolution⋆
Leiden Observatory, Leiden University, PO Box 9513
2300 RA, Leiden, The Netherlands
2 UK Astronomy Technology Center, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
3 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
4 Department of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
5 Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
6 Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán, México, Mexico
Received: 8 August 2014
Accepted: 18 December 2014
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.
Key words: radio lines: ISM / HII regions / ISM: molecules / ISM: jets and outflows / stars: massive
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2015
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