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Induced Star Formation in M17: High Resolution NH3 and IR Observations

Published online by Cambridge University Press:  04 August 2017

M. Felli ,
M. Massi ,
R. Stanga  and
E. Churchwell
M. Felli
Affiliation:
Osservatorio di Arcetri, Florence, Italy
M. Massi
Affiliation:
Osservatorio di Arcetri, Florence, Italy
R. Stanga
Affiliation:
Instituto di Astronomia, Florence, Italy
E. Churchwell
Affiliation:
University of Wisconsin, Madison, USA

Extract

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A VLA radio continuum study of the H II region M17 (Felli, Churchwell and Massi, 1984) has shown the presence of an elongated sharp arc structure in the South Bar of the nebula, in a region of heavy obscuration. The arc has been interpreted as an ionization boundary, viewed edge on, located between the diffuse H II region, to the east, and a dense component of the extended molecular cloud, to the west. About 3″ to the west of this arc, an ultra-compact H II region has been found. This has a shell type structure, a linear diameter of 0.004 pc and probably is the result of induced star formation in the molecular cloud produced by the pressure front preceding the ionization front.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 141 - 142
Copyright
Copyright © Reidel 1987 

References

Felli, M., Churchwell, E., and Massi, M.: 1984, Astron. Astrophys. 136, 53.Google Scholar