ArTéMiS imaging of the filamentary infrared dark clouds G1.75-0.08 and G11.36+0.80: Dust-based physical properties of the clouds and their clumps

Abstract

We imaged the infrared dark clouds (IRDCs) G1.75-0.08 and G11.36+0.80 at 350 $\mu$m and 450 $\mu$m using the ArTéMiS bolometer. These data were used in conjunction with our previous 870 $\mu$m observations with the Large APEX BOlometer CAmera (LABOCA). The clumps in G11.36+0.80 were also observed in the N${}_2$H${}^{+}(1-0)$ transition with the IRAM 30-metre telescope. G1.75-0.08 was found to be composed of two cold ($\sim 14.5$ K), massive (several $\sim 10^3$ M${}_{\odot }$) clumps that are projectively separated by $\sim 3.7$ pc. Both clumps are 70 $\mu$m dark, but they do not appear to be bounded by self-gravity. The G1.75-0.08 filament was found to be subcritical by a factor of $\sim 14$ with respect to its critical line mass. G11.36+0.80 was found to be moderately (by a factor of $\sim 2$) supercritical and composed of four clumps. The dust temperatures of the clumps are $\sim 13-15$ K, and their masses are in the range $\sim 232-633$ M${}_{\odot }$. All the clumps are gravitationally bound. The projected, average separation of the clumps is $\sim 1$ pc. A configuration that is observed in G1.75-0.08, namely two clumps at the ends of the filament, could be the result of gravitational focussing acting along the cloud. The two clumps fulfil the mass-radius threshold for high-mass star formation. Owing to the location of G1.75-0.08 near the Galactic centre ($\sim 270$ pc), environmental effects such as a high level of turbulence, tidal forces, and shearing motions could affect the cloud dynamics. The observed clump separation in G11.36+0.80 can be understood in terms of a sausage instability. The G11.36+0.80 clumps do not lie above the mass-radius threshold for high-mass star formation. The substructure observed in one of the clumps in G11.36+0.80 suggests that the IRDC has fragmented in a hierarchical fashion. This conforms to the filamentary paradigm for Galactic star formation.

arXiv comment16 pages (incl. two appendices), 8 figures, 10 tables, accepted for publication in A&A, abstract abridged for arXiv

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