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SiO Masers in the Star Forming Regions W51 IRS2 and Sgr B2 MD5

Published online by Cambridge University Press:  04 August 2017

N. Ukita ,
T. Hasegawa ,
N. Kaifu ,
K.-I. Morita ,
S. Okumura ,
H. Suzuki ,
M. Ohishi  and
M. Hayashi
N. Ukita
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan
T. Hasegawa
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan
N. Kaifu
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan
K.-I. Morita
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan
S. Okumura
Affiliation:
Dapartment of Astronomy, University of Tokyo, Japan
H. Suzuki
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan
M. Ohishi
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan Dapartment of Astronomy, University of Tokyo, Japan
M. Hayashi
Affiliation:
Dapartment of Astronomy, University of Tokyo, Japan

Extract

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The maser emission of the J = 1-0 lines of SiO in vibrationally excited states has been detected in two regions of massive star formation, W51 IRS2 and Sgr B2 MD5. The SiO masers apparently coincide with strong H2O masers in each source within the uncertainties of < 5″. Their velocity ranges fall within those of the nearest H2O masers (Figure 1). In W51 IRS2 the maser emission is observed only in the v = 2 state, and the upper limit of the v = 1 line (3σ) is 1/15th of the v = 2 line intensity. The v = 1 emission found in Sgr B2 MD5 is five times stronger than the marginally detected v = 2 emission (Figure 2). Their luminosities are comparable to those from the corresponding maser in Orion.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 178
Copyright
Copyright © Reidel 1987