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Massive Star Formation in W49

Published online by Cambridge University Press:  04 August 2017

J. Dreher
Affiliation:
Dept. of Physics, MIT, Cambridge, MA 02139, USA
S. Vogel
Affiliation:
Radio Astron. Lab., U. California, Berkeley, CA 94720, USA
S. Terebey
Affiliation:
HAO, Natl. Ctr. for Atmospheric Research, Boulder, CO 80307, USA
W. J. Welch
Affiliation:
Radio Astron. Lab., U. California, Berkeley, CA 94720, USA

Extract

W49 is the most luminous H II region complex in the galaxy. VLA maps in the continuum reveal a complex of more than two dozen compact HII regions, including a ring-like distribution of a dozen such regions within a volume of 1 pc. In addition to the VLA maps, we have obtained high resolution maps in this field with the Hat Creek Millimeter Interferometer in the following molecular lines: HCO+(1-0), H13CO+(1-0), SiO(v = 0, J = 2-1), SiO(v = 1, J = 2-1), H13CN(1-0), HC15N(1-0), SO2 [8(3,5)-9(2,8)], SO2[8(1,7)-8(0,8)], SO[2(2)-1(1)], and CH3CH2CN[10(1,10)-9(1,9)], all near 3 mm wavelengh. These maps will be discussed. The HCO+distribution corresponds to the larger scale structures observed in the continuum maps. In contrast the SO and SiO sources are quite compact. Using the detailed molecular line results obtained in the ORION/KL region as a guide, we are able to identify these latter sources as regions in which the star formation is at an earlier stage, regions where there are outflows.

Type
I. Star Forming Processes in the Solar Neighborhood
Copyright
Copyright © Reidel 1987 
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