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A collimated jet and an infalling-rotating disk in G192 traced by H2O maser emission

Published online by Cambridge University Press:  01 March 2007

Hiroshi Imai ,
Toshihiro Omodaka ,
Tomoya Hirota ,
Tomofumi Umemoto ,
Kazuo Sorai  and
Tetsuro Kondo
Hiroshi Imai
Affiliation:
Department of Physics, Faculty of Science, Kagoshima University, Japan email: hiroimai@sci.kagoshima-u.ac.jp
Toshihiro Omodaka
Affiliation:
Department of Physics, Faculty of Science, Kagoshima University, Japan email: hiroimai@sci.kagoshima-u.ac.jp
Tomoya Hirota
Affiliation:
Mizusawa VERA Observatory Mitaka Office, National Astronomical Observatory, Japan
Tomofumi Umemoto
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory, Japan
Kazuo Sorai
Affiliation:
Division of Physics, Graduate School of Science, Hokkaido University, Japan
Tetsuro Kondo
Affiliation:
Kashima Space Research Center, National Institute of Information and Communication Technology, Japan
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Abstract

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We present H2O masers associated with the massive-star forming region G192 observed with the Japan VLBI network since the year 2005, The spatio-kinematical structure of the maser feature clusters has well persisted since previous observations, in which the masers are associated with two young stellar objects (YSOs) separated by ~1200 AU and expected to be associated with a highly-collimated bipolar jet and an infalling-rotating disk in the northern and southern YSOs, respectively. We estimated a jet speed of ~100 km s−1 and re-estimated a dynamical age of the whole jet to be 5.6×104 years. The spatial distribution of maser Doppler velocities found during the previous and present observations, relative proper motions of H2O maser features in the southern cluster found in the present observations, a relative bulk motion between the two maser clusters are well explained by a model of an infalling-rotating disk with a radius of ~1000 AU and a central stellar mass of ~8 M⊙.

Keywords

masersstars:mass accretionindividual (G192.16–3.84)ISM:jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 340 - 341
Copyright
Copyright © International Astronomical Union 2008

References

Imai, H., Omodaka, T., Hirota, T., Umemoto, T., Sorai, K., & Kondo, T. 2006, PASJ, 58, 883CrossRefGoogle Scholar
Shepherd, D. S. et al. 2004 ApJ, 614, 211CrossRefGoogle Scholar
Shepherd, D. S., Claussen, M. J., & Kurtz, S. E. 2001, Science, 292, 1513CrossRefGoogle Scholar
Shepherd, D. S., & Kurtz, S. E. 1999, ApJ 523, 690CrossRefGoogle Scholar