The Giant Molecular Cloud associated with RCW 106 -- A 1.2 mm continuum mapping study

TL;DR

This study maps dust emission in the RCW 106 molecular cloud at 1.2 mm, revealing 95 clumps, new features, and insights into star formation, mass distribution, and cloud structure.

Contribution

It provides high-resolution dust continuum mapping of RCW 106, identifying new emission features and analyzing the clump mass spectrum with independent methods.

Findings

95 dust clumps identified in the GMC

Clump mass spectrum index of 1.6±0.3

Approximately 10% of sources show signs of high-mass star formation

Abstract

We have mapped the dust continuum emission from the molecular cloud covering a region of 28pcx94pc associated with the well-known HII region RCW 106 at 1.2 mm using SIMBA on SEST. The observations, having an HPBW of 24" (0.4 pc), reveal 95 clumps. Owing to the higher sensitivity to colder dust and higher angular resolution the present observations identify new emission features and also show that most of the IRAS sources in this region consist of multiple dust emission peaks. The detected millimeter sources (MMS) include on one end the exotic MMS5 (associated with IRAS 16183-4958, one of the brightest infrared sources in our Galaxy) and the bright (and presumably cold) source MMS54, with no IRAS or MSX associations on the other end. Around 10% of the sources are associated with signposts of high mass star formation activity. Assuming a uniform dust temperature of 20 K we estimate the total mass of the GMC associated with RCW 106 to be ~10^5\msun. The constituent millimeter clumps cover a range of masses and radii between 40 to 10^4 \msun and 0.3 to 1.9 pc. Densities of the clumps range between (0.5-6) 10^4 cm^{-3}. We have decomposed the continuum emission into gaussian and arbitrary shaped clumps using the two independent structure analysis tools gaussclumps and clumpfind respectively. The clump mass spectrum was found to have an index of 1.6+-0.3, independent of the decomposition algorithm used. The index of the mass spectrum for the mass and length scales covered here are consistent with results derived from large scale CO observations.