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Fig. 13.

image

Spectra of individual clumps #1.2 S (left panel) and #1.2 N (right panel), extracted from our PdBI CO(4–3) data cube using 0.6″ × 0.6″ apertures, and corrected for gravitational magnification. Clump #1.2 N is well fitted with a single Gaussian function (red curve), while #1.2 S exhibits a secondary component, blueshifted with respect to the systemic component (blue curves), which we interpret as the signature of a stellar wind.

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