Similar to Fig. 5, but for the thermally supercritical filament B211/B213 in the Taurus cloud at d ~ 140 pc (cf. Palmeirim et al. 2013). The mean line mass of the filament is ⟨M_line⟩ ~ 30M_⊙/pc ≫M_line,crit, as shown by the dotted horizontal line in panel b). The median relative amplitude of the line-mass fluctuations is . We note the spike features corresponding to the positions of dense cores along the filament and capturing non-linear density perturbations. In panel c), the power-law fits to the power spectra P_obs(s) and P_true(s) have logarithmic slopes −2.2 ± 0.2 and −1.9 ± 0.3, respectively. The best power-law fit to P_true(s) is unchanged if only angular frequencies up to = 1.5 arcmin^-1 are considered. (This figure is available in color in electronic form.)