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VLA Observations of H2O Masers in the Class 0 Protostar S106FIR

Published online by Cambridge University Press:  12 April 2016

R. Furuya ,
R. Kawabe ,
M. Saito ,
T. Umemoto  and
Y. Kitamura
R. Furuya
Affiliation:
The Graduate Univ. for Advanced Studies & Nobeyama Radio Observatory, Japan
R. Kawabe
Affiliation:
National Astronomical Observatory, Japan
M. Saito
Affiliation:
National Astronomical Observatory, Japan
T. Umemoto
Affiliation:
National Astronomical Observatory, Japan
Y. Kitamura
Affiliation:
Institute of Space and Astronautical Science, Japan

Abstract

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We measured relative positions of the 22 GHz H2O maser components toward the class 0 protostar S106FIR with the VLA. Two clusters of H2O masers were found. The separation between these clusters is approximately 50 AU at position angle = 73° and each cluster is spread over about 10–20 AU The size of the S106FIR maser clusters is unusually compact compared with other known H2O masers associated with outflows of forming stars. The maser emission appears to originate from MHD driven outflow very close to the star.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 164: Radio Emission from Galactic and Extragalactic Compact Sources , 1998 , pp. 247 - 248
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Bachiller, R. 1996. ARA&A, 34, 111–154.Google Scholar
Hayashi, S.S., et al. 1990. ApJ, 354, 242–246.Google Scholar
Mangum, J.G., & Wootten, A. 1994. BAAS, 26, 1454.Google Scholar
Richer, J.S., et al. 1993. MNRAS, 262, 839–851.Google Scholar