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VLBI Mapping of 43 GHz SiO Emission Associated with IRc2 in Orion-KL

Published online by Cambridge University Press:  03 August 2017

L. J. Greenhill ,
J. M. Moran ,
M. J. Reid ,
C. R. Predmore ,
G. C. McIntosh  and
A. E. E. Rogers
L. J. Greenhill
Affiliation:
Center for Astrophysics, Cambridge, MA
J. M. Moran
Affiliation:
Center for Astrophysics, Cambridge, MA
M. J. Reid
Affiliation:
Center for Astrophysics, Cambridge, MA
C. R. Predmore
Affiliation:
University of Massachusetts, Amherst, MA
G. C. McIntosh
Affiliation:
University of Massachusetts, Amherst, MA
A. E. E. Rogers
Affiliation:
Haystack Observatory, Westford, MA

Extract

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Information on the structure of the molecular flow within 1″ of IRC-2, in Orion-KL, is sparse. Measurements of the continuum at 7.8μ and 12.5μ show a disk of size and suggest that the center of the disk may be dust free (Lester et al. 1985). Aperture synthesis mapping of water maser shell features (Sylber 1986) has provided information on the scale. Smaller scales can be studied by mapping SiO maser emission. We observed the 43 GHz, v=1, J = 1 → 0, transition of SiO using a 2 station interferometer with a 74 km baseline between Haystack Observatory, Westford, MA and Five College Radio Observatory, New Salem, MA. The fringe spacing was 20 milliarcseconds (mas) and the velocity resolution was 0.25 km-s−1. Our results provide the highest resolution view to date of what is likely to be the inner of IRC-2.

Type
Galactic
Information
Symposium - International Astronomical Union , Volume 129: The Impact of VLBI on Astrophysics and Geophysics , 1988 , pp. 253 - 254
Copyright
Copyright © Reidel 1988 

References

Genzel, R. 1985 in Masers, Molecules and Mass Outflows in Star Forming Regions, ed. Haschick, A., 233.Google Scholar
Genzel, R., Reid, M. J., Moran, J. M., and Downes, D. 1981, Ap. J., 244, 884.Google Scholar
Genzel, R., Moran, J. M., Lane, A. P., Predmore, C. R., Ho, P. T. P., Hansen, S. S., and Reid, M. J. 1979, Ap. J. (Letters), 231, L73.CrossRefGoogle Scholar
Lane, A. P. 1982, , University of Massachusetts, Amherst.Google Scholar
Lester, D. F., Becklin, E. E., Genzel, R., and Wynn-Williams, C. G., 1985, A. J., 90, 2331.Google Scholar
Moran, J. M., Garay, G., Reid, M. J. 1987, in preparation.Google Scholar
Plambeck, R. L., Wright, M. C. H., Welch, W. J., Bieging, J. H., Baud, B., Ho, P. T. P., and Vogel, S. N. 1982, Ap. J., 259, 617.Google Scholar
Sylber, M. 1986, private communication.Google Scholar
Vogel, S. N., Bieging, J. H., Plambeck, R. L., Welch, W. J., and Wright, M. C. H. 1985, Ap. J., 296, 600.Google Scholar
Wright, M. C. H. and Plambeck, R. L. 1983, Ap. J. (Letters), 267, L115.Google Scholar