Extended Data Fig. 5: Distribution of interstellar filament widths in observations and theory.
Filament width distribution measured from observations in the IC5146, the Aquila and the Polaris molecular clouds shown as the orange histogram, together with the theoretical prediction based on the sonic scale (blue line; see Supplementary Information for the details of this function). The theoretical prediction is not a fit; instead the peak position is set to x0 = 0.1 parsec and the log-normal standard deviation, σx = 0.105, is determined by the width of the sonic-scale transition measured in Fig. 2.
