Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apjs..124..439k&link_type=abstract
The Astrophysical Journal Supplement Series, Volume 124, Issue 2, pp. 439-463.
Astronomy and Astrophysics
Astronomy
27
Ism: H Ii Regions, Ism: Individual (Ngc 6334), Ism: Kinematics And Dynamics, Radio Lines: Ism, Stars: Formation
Scientific paper
We present millimeter- and centimeter-wave spectroscopic observations of the southern massive star formation region NGC 6334. The cloud has been mapped in several transitions of CO, 13CO, CS, and NH3. The molecular gas shows a complex structure of filaments, in which the massive star formation occurs, and bubbles, some of which contain photodissociated gas. There is an anticorrelation between the presence of dense gas and the 6 cm radio flux: the hottest stars, with the hardest FUV radiation, have dispersed the dense gas from which they formed, whereas the cooler stars have not yet been able to do so. There is a velocity gradient along the star-forming ridge such that the radial velocity peaks in the center of the ridge. Several blueshifted emission features were discovered, one of which was identified with the ``3-kpc'' arm of the Galaxy. Excitation model calculations were used to determine the physical conditions of the molecular gas in NGC 6334. The average kinetic temperature, hydrogen volume, and column densities at the continuum sources are as follows: Tk&=56+/-11 K, log nH2 (cm-3)=3.5+/-0.3, and NH2 (1022 cm-2)=7+/-4, respectively. The properties of the molecular gas are compared to those in other massive star-forming clouds to determine that NGC 6334 is representative of massive star-forming regions in the Galaxy and can therefore be used to test the predictions of the theoretical models of photodissociation regions. The properties of the individual sites of star formation in the cloud are also discussed.
Jackson James M.
Kraemer Kathleen E.
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