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Structure of SiO masers in Orion-KL

Published online by Cambridge University Press:  03 August 2017

Sheperd Doeleman ,
Colin Lonsdale ,
Paul Kondratko ,
Whitney Raas  and
C. Read Predmore
Sheperd Doeleman
Affiliation:
MIT Haystack Observatory, Off Route 40, Westford, MA. 01886, USA
Colin Lonsdale
Affiliation:
MIT Haystack Observatory, Off Route 40, Westford, MA. 01886, USA
Paul Kondratko
Affiliation:
MIT Haystack Observatory, Off Route 40, Westford, MA. 01886, USA
Whitney Raas
Affiliation:
MIT Haystack Observatory, Off Route 40, Westford, MA. 01886, USA
C. Read Predmore
Affiliation:
University of Massachusetts, Dept. of Astronomy, 619 Lederle Graduate Research Center, Amherst, MA 01003, USA

Abstract

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The Orion-KL nebula is the closest (450pc) site of high-mass star formation and exhibits powerful outflows associated with protostars. It is also one of only three known star forming regions to exhibit SiO maser emission. Emission in three SiO maser transitions (v=1 J=1 → 0, v=1 J=2 → 1, and v=2 J=1 → 0) imaged by VLBI exhibits an “X” morphology suggesting that the Orion masers form along the outlines of two opposing conical outflows to the NW and SE. At the center of this “X”, VLA observations find emission from an HII region presumably associated with a young star whose wind drives the outflow. The SiO masers probably form along the interface between the stellar wind and surrounding parent cloud. We find that SiO maser emission from different transitions preferentially occurs at different radii from the central star implying that the masers are tracers for physical conditions in the wind-cloud interaction region. On the smallest scales, some individual maser features in each transition overlap both spatially and in velocity providing strong evidence that more than one transition can mase within the same volume of gas.

Type
Part 2. Stellar Masers
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 290 - 293
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

Barvainis, R. E. 1984, ApJ, 279, 358 CrossRefGoogle Scholar
Barvainis, R. E. & Predmore, C.R. 1985, ApJ, 288, 694 CrossRefGoogle Scholar
Bujarrabal, V. 1994, A&A, 285, 953 Google Scholar
Chernin, L.M. & Wright, M.H. 1996, ApJ, 467, 676 CrossRefGoogle Scholar
Desmurs, J. F., Bujarrabal, V., Colomer, F., & Alcolea, J. 2000, A&A, 360, 189D Google Scholar
Doeleman, S.S., Lonsdale, C.J., & Pelkey, S. 1999, ApJ, 510, L55 Google Scholar
Greenhill, L.J., Gwinn, C.R., Schwartz, C., Moran, J.M., & Diamond, P.J. 1998, Nature, 396, 650 CrossRefGoogle Scholar
Lockett, P. & Elitzur, M. 1992, ApJ, 399, 704 CrossRefGoogle Scholar
McIntosh, G.C. & Predmore, C.R. 1993, ApJ, 404, L71 Google Scholar
Menten, K.M. & Reid, M.J. 1995, ApJ, 445, L157 CrossRefGoogle Scholar
Plambeck, R.L, Wright, M.C.H., & Carlstrom, J.E. 1990, ApJ, 348, L65 CrossRefGoogle Scholar
Stolovy, S. R., Burton, M. G., Erickson, E. F., Kaufman, M. J., Chrysostomou, A., Young, E. T., Colgan, S. W. J., Axon, D. J., Thompson, R. I., Rieke, M. J., & Schneider, G. 1998, ApJ, 492, L151 CrossRefGoogle Scholar