Hostname: page-component-78c5997874-m6dg7 Total loading time: 0 Render date: 2024-11-10T22:11:50.999Z Has data issue: false hasContentIssue false
  • English
  • Français

Dynamics of jet/outflow driven by high-mass young stellar object revealed by KaVA 22 GHz water maser observations

Published online by Cambridge University Press:  16 July 2018

Jungha Kim ,
Tomoya Hirota ,
Kee-Tae Kim ,
Koichiro Sugiyama  and
KaVA Science Working Group for Star-formation
Jungha Kim
Affiliation:
Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan email: jungha.kim@nao.ac.jp Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Tomoya Hirota
Affiliation:
Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan email: jungha.kim@nao.ac.jp Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Kee-Tae Kim
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdaero, Yuseong, Daejeon 34055, Korea
Koichiro Sugiyama
Affiliation:
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have started survey observations of the 22 GHz water maser sources associated with high-mass young stellar objects (HM-YSOs) as a part of the KaVA (KVN and VERA Array) large program (LP). The aim of our LP is to understand dynamical evolution of jets/outflows from HM-YSOs by analyzing 3D velocity structures of water maser features. In the first year (2016-2017), an imaging survey toward 25 HM-YSOs has been conducted and the 22 GHz water masers are detected toward 21 sources. Spatial distributions of maser features for individual sources are mapped. To complement physical properties in the vicinity of HM-YSOs, we have carried out ALMA cycle 3 observations of thermal molecular lines and continuum emissions toward 11 selected samples. Summary of the KaVA first year observations and the initial results from the ALMA toward one of our targets, G25.82-0.17, are reported.

Keywords

ISM: kinematics and dynamicsISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S336: Astrophysical Masers: Unlocking the Mysteries of the Universe , September 2017 , pp. 303 - 304
Copyright
Copyright © International Astronomical Union 2018 

References

Green, J. A. & McClure-Griffiths, N. M., 2011, MNRAS, 417, 2500CrossRefGoogle Scholar
Shirley, Y. L., Ellsworth-Bowers, T. P., Svoboda, B., et al., 2013, ApJS, 209, 2CrossRefGoogle Scholar
Urquhart, J. S., Morgan, L. K., Figura, C. C., et al., 2011, MNRAS, 418, 1689CrossRefGoogle Scholar