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 k_fil ∼ (0.6/θ_{fil − width})∼0.45 arcmin⁻¹ corresponding to a filament width of θ_{fil − 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 k_min <  k <  1.5 k_fil is ∼0.045.