Large-Scale NH3 Observations toward the Galactic Star-Forming Regions I. W51 Molecular Cloud Complex

Details Large-Scale NH3 Observations toward the Galactic Star-Forming Regions I. W51 Molecular Cloud Complex Large-Scale NH3 Observations toward the Galactic Star-Forming Regions I. W51 Molecular Cloud Complex

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008pasj...60.1285s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.60, No.6, pp.1285--1296

Astronomy and Astrophysics

Astronomy

1

Ism: Clouds - Ism: Individual (W51) - Stars: Formation

Scientific paper

Large-area observations of dense molecular gas were made in NH3 (J, K) = (1, 1), (2, 2), and (3, 3) inversion lines with 4'.5 resolution toward the molecular cloud complex of the W51 region. The observations were a part of a NH3 survey of the Galactic star-forming regions using the Tomakomai 11-m radio telescope. NH3 (J, K) = (1, 1) and (2, 2) emission was detected in the W51 A and B complexes, while the detection of (J, K) = (2, 2) emission was marginal in W51 B. The rotation temperature was ˜ 40K in the central part of the W51 A complex, while being ˜ 20K in the other positions. A weak correlation is found that the ortho-to-para ratio decreases with increasing the rotation temperature, the far-infrared luminosity and the index of the star-formation efficiency. This tendency is explained if star formation has continued for more than the time scale of the transformation between ortho- and para-NH3: active star formation on a large scale, such as the interaction of molecular clouds with a spiral arm, has made the molecular gas warmer, even in a scale of ˜ 10pc, and the proceeding transformation has made the ortho-to-para ratio lower.

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