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Fig. 3


Examples of NH3(1,1) spectra at ten positions in the cloud, plotted surrounding the H2 column density derived from the NH3 emission (discussed later in Sect. 3.2). The model fit is plotted over each spectrum in red, whilst the residual of the two is plotted in the bottom panel with the standard deviation quoted in mJy beam−1. Regions of specific interest include those where the velocity width is seen to increase (spectra 1 and 6), positions where the centroidvelocity changes as a filament meets the central hub (spectra 3, 4 and 7) and the large starless core MM2 (spectrum 8). It is clear that there is only a single velocity component everywhere in the cloud, with some lines being narrow enough to start resolving further hyperfine components (spectrum 10), and some showing the tell-tale signs of the cloud identified by Peretto et al. (2014) at a V sys = 54 kms−1 that likely overlaps in projection with the north-east filament (spectrum 1 and 2).

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