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Japanese VLBI network observations of 6.7-GHz methanol masers II. Results

Published online by Cambridge University Press:  01 March 2007

Koichiro Sugiyama ,
Kenta Fujisawa ,
Mareki Honma ,
Akihiro Doi ,
Nanako Mochizuki ,
Yasuhiro Murata  and
Yasuko Isono
Koichiro Sugiyama
Affiliation:
Faculty of Science, Yamaguchi University, 1677-1 Yoshida, Yamaguchi, Yamaguchi 753-8512
Kenta Fujisawa
Affiliation:
Faculty of Science, Yamaguchi University, 1677-1 Yoshida, Yamaguchi, Yamaguchi 753-8512
Mareki Honma
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588
Akihiro Doi
Affiliation:
The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510
Nanako Mochizuki
Affiliation:
The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510
Yasuhiro Murata
Affiliation:
The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510
Yasuko Isono
Affiliation:
Faculty of Science, Yamaguchi University, 1677-1 Yoshida, Yamaguchi, Yamaguchi 753-8512
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Abstract

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We are using a Japanese VLBI network (JVN) for VLBI observations of 6.7-GHz methanol masers associated with massive star-forming regions. Here we present results for Cepheus A (Cep A) from observations taken on September 9, 2006. The distribution of the maser spots indicates either a spherical bubble or a disk having an inclination of several tens degree. We construct a disk model with an inclination of ~70° and a radius of ~700 AU. From a luminosity of 1.7 × 104L⊙ for a source observed in this region, the excitation of the maser is probably radiative.

Keywords

masersstars: formationH II regionsISM: individual (Cepheus A)

References

Cragg, D. M., Sobolev, A. M., & Godfrey, P. D. 2002, MNRAS, 331, 521CrossRefGoogle Scholar
Doi, A., et al. 2006, Proc. 8th European VLBI Network Symposium, PoS(8thEVN) 071Google Scholar
Johnson, H. L. 1957, ApJ, 126, 121CrossRefGoogle Scholar
Pestalozzi, M. R., Elitzur, M., Conway, J. E., & Booth, R. S. 2004, ApJ, 603, L113CrossRefGoogle Scholar
Pestalozzi, M. R., Minier, V., & Booth, R. S. 2005, A&A, 432, 737Google Scholar
Torrelles, J. M., Gomez, J. F., Rodriguez, L. F., Curiel, S., Ho, P. T. P., & Garay, G. 1996, ApJ, 457, L107CrossRefGoogle Scholar
Walsh, A. J., Hyland, A. R., Robinson, G., & Burton, M. G. 1997, MNRAS 291, 261CrossRefGoogle Scholar