Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...423..320h&link_type=abstract
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 423, no. 1, p. 320-325
Astronomy and Astrophysics
Astrophysics
18
Interstellar Matter, Molecular Clouds, Star Formation, Stellar Cores, Stellar Rotation, Brightness Distribution, Brightness Temperature, H Ii Regions, Millimeter Waves
Scientific paper
Using the Owens Valley Radio Observatory millimeter-wave interferometer, the compact molecular cloud core surrounding the H II region G10.60-0.4 has been resolved in the C(18)O J = 1-0 transition. Since this line is most likely optically thin, it is an excellent tracer of the total column density. We find a centrally condensed and flattened (12.6 sec x 4.2 sec ; 0.3 pc x 0.1 pc) core, which is rotating rapidly with a substantial velocity gradient (17 +/- 2 km/s pc) along the major axis. The core is quite bright (greater than 10K), dense (greater than (106/cu cm), massive (103 solar mass), and embedded in a more extended (greater than 60 seconds) envelope. There is no evidence for absorption, implying that the C(18)O emitting gas is both optically thin and substantially hotter than the equivalent continuum temperature at 3 mm. The systemic velocity of the rotating core is -2.5 +/- 0.5 km/s, the same as the systemic velocity of the extended cloud.
Ho Paul T. P.
Terebey Susan
Turner Jean L.
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