[Previous] | [Session 71] | [Next]
J. A. Eisner (Harvard University), J. R. Herrnstein (NRAO), L. J. Greenhill (Harvard-Smithsonian CfA), K. M. Menten (MPIfR)
The W51-IRS2 star-forming region is one of only three in which SiO maser emission has been detected. In contrast, SiO maser sources occur in the circumstellar envelopes of tens of late-type stars. We present the results of sensitive, high angular resolution observations of W51-IRS2 made with the VLA in its two largest configurations, at 7 mm and 1 cm wavelengths. The SiO maser emission is coincident with a known luminous cluster of water masers, although no corresponding radio continuum source is detected. The SiO emission has a linear spatial structure and may trace an outflow from an obscured protostar, on scales of approximately 200 AU. The proposed model in consistent with the morphology of the brightness distribution of water masers.
The author(s) of this abstract have provided an email address for comments about the abstract: jeisner@cfa.harvard.edu