Other
Scientific paper
Aug 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...413..571s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 413, no. 2, p. 571-581.
Other
47
Mass Distribution, Molecular Clouds, Molecular Spectra, Star Formation, Astronomical Models, Astronomical Spectroscopy, Electron Transitions, Emission Spectra
Scientific paper
A multitransitional study of the W49N molecular cloud core has been carried out in seven rotational lines of CS and C(S-34), ranging in excitation from J = 3-2 to J = 10-9. The cloud core has been found to consist primarily of three dense molecular clumps, of size 0.4-1.0 pc, located approximately along an axis at P.A. 56 deg on the plane of the sky. The clumps' local densities are 2-6 x 10 exp 6/cu cm, and their masses a few 10 exp 4 solar masses each, yielding a total core mass of about 10 exp 5 solar masses. The two outer clumps are receding from us at an LSR velocity of 12 km/s, but the central clump is instead moving away at only 4 km/s, indicating that two different molecular clouds are present toward W49A. Absorption studies place the 12 km/s gas closer to us than the 4 km/s gas, implying that these two molecular clouds are converging upon each other. In addition, the central CS clump is found to be spinning rapidly in a direction counter both to Galactic rotation and to the direction inferred earlier from recombination line observations of the W49A compact H II regions. The hypothesis of global molecular cloud collapse is inconsistent with our new molecular line data. Instead, the molecular gas kinematics suggest that the enhanced O-star formation rate in W49N has been triggered by a cloud-cloud collision.
Guesten Rolf
Schulz André
Serabyn Eugen
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