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Title:
VLBI observations of the SiO maser in Orion
Authors:
Genzel, R.; Moran, J. M.; Lane, A. P.; Predmore, C. R.; Ho, P. T. P.; Hansen, S. S.; Reid, M. J.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AC(Massachusetts, University, Amherst, Mass.), AD(Massachusetts, University, Amherst, Mass.), AE(Massachusetts, University, Amherst, Mass.), AF(National Radio Astronomy Observatory, Charlottesville, Va.), AG(National Radio Astronomy Observatory, Charlottesville, Va.)
Publication:
Astrophysical Journal, Part 2 - Letters to the Editor, vol. 231, July 15, 1979, p. L73-L76. (ApJL Homepage)
Publication Date:
07/1979
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Interstellar Masers, Orion Nebula, Protostars, Silicon Oxides, Stellar Envelopes, Very Long Base Interferometry, Water Masers, Infrared Astronomy, Millimeter Waves, Stellar Radiation, Variability
DOI:
10.1086/183007
Bibliographic Code:
1979ApJ...231L..73G

Abstract

VLBI observations of the v = 1, J = 1 - 0 SiO maser transition at 43 GHz from the Kleinmann-Low (KL) nebula in Orion are reported. The blueshifted (-6 km/s) and redshifted (19 km/s) 'shell' features are found to originate from the same position on the sky, indicating that these features are associated with a single star. It is suggested that the SiO, H2O, and possibly OH lines at about -6 and +16 km/s probably arise from the same source in the Orion-KL region. The variability of the SiO emission and IR emission from the 'shell source' are discussed. A model is considered in which the maser emission originates from the front and the back of a thick expanding (or contracting) circumstellar shell.

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