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Proper motions of water masers: W 51 North, Main, and South

Published online by Cambridge University Press:  03 August 2017

Hiroshi Imai ,
Tetsuo Sasao ,
Osamu Kameya ,
Teruhiko Watanabe ,
Toshihiro Omodaka ,
Masanori Nishio ,
Yoshiharu Asaki  and
Jun-Ichi Nakajima
Hiroshi Imai
Affiliation:
VERA Project Office, NAOJ, Mitaka, Tokyo 181-8588, Japan
Tetsuo Sasao
Affiliation:
VERA Project Office, NAOJ, Mitaka, Tokyo 181-8588, Japan
Osamu Kameya
Affiliation:
VERA Project Office, NAOJ, Mitaka, Tokyo 181-8588, Japan
Teruhiko Watanabe
Affiliation:
Dept. of Physics, Kagoshima University, Kagoshima 890-0065, Japan
Toshihiro Omodaka
Affiliation:
Dept. of Physics, Kagoshima University, Kagoshima 890-0065, Japan
Masanori Nishio
Affiliation:
Dept. of Physics, Kagoshima University, Kagoshima 890-0065, Japan
Yoshiharu Asaki
Affiliation:
Institute Space and Astronautical Science, Sagamihara, Kanagawa 229-0022, Japan
Jun-Ichi Nakajima
Affiliation:
KSRC, Communications Research Laboratory, Kashima, Ibaraki 314-0012, Japan

Abstract

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We describe the proper motion measurements of water masers in the massive-star forming region W 51A and the analysis of the 3-D kinematics in three maser clusters of W 51A. We found a systematic expanding motion in one of the clusters named W 51 North, while no systematic motion was detected in other two clusters named W 51 Main and South. The 3-D motions of the clusters relative to the position reference feature in W 51 North indicate a separating motion between the W 51 North and the W 51 Main/South clusters. We estimated the distance to W 51 North as to be 6.7±2.1 kpc on basis of the statistical parallax and the model fitting methods.

Type
Part 1. Star Formation
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 88 - 91
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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