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We present high-resolution (sub-parsec) observations of a giant molecularcloud in the nearest star-forming galaxy, the Large Magellanic Cloud. ALMA Band6 observations trace the bulk of the molecular gas in $^{12}$CO(2-1) and highcolumn density regions in $^{13}$CO(2-1). Our target is a quiescent cloud (PGCCG282.98-32.40, which we refer to as the "Planck cold cloud" or PCC) in thesouthern outskirts of the galaxy where star-formation activity is very low andlargely confined to one location. We decompose the cloud into structures usinga dendrogram and apply an identical analysis to matched-resolution cubes of the30 Doradus molecular cloud (located near intense star formation) forcomparison. Structures in the PCC exhibit roughly 10 times lower surfacedensity and 5 times lower velocity dispersion than comparably sized structuresin 30 Dor, underscoring the non-universality of molecular cloud properties. Inboth clouds, structures with relatively higher surface density lie closer tosimple virial equilibrium, whereas lower surface density structures tend toexhibit super-virial line widths. In the PCC, relatively high line widths arefound in the vicinity of an infrared source whose properties are consistentwith a luminous young stellar object. More generally, we find that the smallestresolved structures ("leaves") of the dendrogram span close to the full rangeof line widths observed across all scales. As a result, while the bulk of thekinetic energy is found on the largest scales, the small-scale energetics tendto be dominated by only a few structures, leading to substantial scatter inobserved size-linewidth relationships.

ALMA Observations of a Quiescent Molecular Cloud in the Large Magellanic Cloud