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Fig. 6.

image

Panel a: Herschel/SPIRE 250 μm image of the Aquila cloud at the native resolution of 182. Panel b: noise-subtracted and beam-corrected power spectrum of the image shown in panel a over the range of angular frequencies 0.025 arcmin−1 <  k <  2 arcmin−1 (black curve). The red curve shows the best fit power-law model over this frequency range, which has a logarithmic slope γ = −2.26 ± 0.1. The vertical dashed line marks the angular frequency kfil ∼ (0.6/θfil − width)∼0.45 arcmin−1 corresponding to a filament width of θfil − width =79 ″ (FWHM), i.e., 0.1 pc at a distance of 260 pc. Panel c: residuals between the best power-law fit and the power spectrum data points (triangle symbols). The of the residuals between kmin <  k <  1.5 kfil is ∼0.045.

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