tokens: orders, which yields a sufficient number of data points for our analysis and still benefits from a low-dimensional covariance. The fact that we do not find a decrease of parameter uncertainty with increasing number of orders shows that the first few orders indeed contain all the relevant information (see Fig. 7 for more details). The measured data points for both angular intervals are presented in Fig. 8 . Unlike correlation function measurements, these Υ data points cannot be interpreted easily. However, it is clear that in the large-scale interval the model (see Section 2 ) is a very good fit to the data regardless of the cosmological parameters used. 4 This is not the case for the smaller scale interval, where one of the clustering data points is several σ away from the best-fitting model. Clearly, the assumption of linear bias on these non-linear scales is not valid for the clustering data. This is partly due to the small uncertainties in these measurements as well as the fact that we neglect the model uncertainties. As can be seen in Fig. 9 , a change of b of about 5 per cent within this interval would already be enough to reconcile the data with the model. If model uncertainties had been included in this figure, it is likely that data and model would be in line again. Another possible explanation of the discrepancy between data and model in this case could be that the fiducial cosmology is wrong. Furthermore, we also investigate if an indication for a scale-dependent bias can be found in the γ t (θ) data in Fig. 10 and find no such preference. Figure 7. Left: the measured parameter values as a function of maximum Υ-order n for b and r . No significant difference in the values is visible, from which we conclude that the data compression is indeed working and only a few orders contain all the information from the measured signals. Right: the parameter uncertainty in per cent for b and r , again as a function of n . Here, we do not find a significant difference, which again shows that the data compression of Υ( n ) is robust. Figure 8. The top panels show the measured Υ gm and Υ gg and the best fit using one of the two cosmologies. The magenta and dark blue lines are the connections between the predicted data points using the Planck or the CFHTLenS cosmology. In the bottom panels, we show the residuals (Υ obs − Υ model )/ΔΥ obs , where ΔΥ obs is the uncertainty in the measured Υ. Left: measurements for the 3-20 arcmin interval. Clearly, on these scales the model we adopt to describe the galaxy bias is not a good description of the data shown here, especially the clustering data. For more details, see Section 3.4 Right: measurements for the 20-70 arcmin interval. Figure 9. Top: the angular correlation function within the small-scale interval, the corresponding model for b = 1, and the best-fitting model. This best-fitting model has been determined from a joint fit of Υ gm and Υ gg . Bottom: the square root of the ratio between the
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