Comparison of projected clustering signal measurements in PAUS W3 and in spectroscopic GAMA data, summarised as fits of the simple, 2-parameter (amplitude A at r_p = 1 h⁻¹ Mpc, and slope γ) power law given by Eq. (A.1). Fits are made via the non-linear least squares method, in the range 0.1 < r_p < 18 h⁻¹ Mpc, and using full jackknife covariances (Sect. 4.3). All measured clustering signals feature heavily correlated r_p-scales, sometimes resulting in poor goodness-of-fit, thus these points should be taken with moderation. Red (blue) galaxy correlations are shown in the left-hand (right-hand) column, with GAMA correlations given by gold stars with red (blue) outlines. PAUS correlations from each of our various configurations (changing Π-binning, randoms and photo-z selection) are denoted by markers and colours, as indicated by the legend.