654 GHz Continuum and C18O (6-5) Observations of G240.31+0.07 with the Submillimeter Array

Details 654 GHz Continuum and C18O (6-5) Observations of G240.31+0.07 with the Submillimeter Array 654 GHz Continuum and C18O (6-5) Observations of G240.31+0.07 with the Submillimeter Array

2006-11-12

arxiv.org/abs/astro-ph/0611366v1

Astrophys.J.654:L87-L90,2006

Astronomy and Astrophysics

Astrophysics

12 pages, 2 tables, 3 figures, accepted by the Astrophysical Journal Letters

Scientific paper

10.1086/510715

We report a dual-band observation at 223 and 654 GHz (460 micron) toward an ultracompact (UC) HII region, G240.31+0.07, with the Submillimeter Array. With a beam size of 1"5 X 0"8, the dust continuum emission is resolved into two clumps, with clump A coincident well with an H2O maser and the UC HII region. The newly discovered clump, B, about 1"3 (~8.3 X 10^3 AU) to the southwest of clump A, is also associated with H2O masers and may be a more recent star-forming site. The continuum flux densities imply an opacity spectral index of \beta = 1.5 +- 0.3, suggestive of a value lower than the canonical 2.0 found in the interstellar medium and in cold, massive cores. The presence of hot (~100 K) molecular gas is derived by the brightness ratio of two H2CO lines in the 223 GHz band. A radial velocity difference of 2.5 +- 0.4 km/s is found between the two clumps in C18O (6-5) emission. The total (nebular and stellar) mass of roughly 58 Msun in the central region is close to, but not by far larger than, the minimum mass required for the two clumps to be gravitationally bound for binary rotation. Our continuum data do not suggest a large amount of matter associated with the H2 knots that were previously proposed to arise from a massive disk or envelope.

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