Left: power-law fitting of the W₀ power spectrum. Upper panel: data (blue crosses), fit result (thick solid line) plotted over the fitted domain, power law convolved with the Gaussian beam (dotted line) extrapolated to all spatial frequencies, noise model (dashed line). Lower panel: residuals. The scale in the Fourier space is given in UV distance as for interferometric observations, which enables us to visually relate the resolution and the telescope diameter. Right: same results, except for the W₁ power spectrum.