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tokens: modelling of the full-shape anisotropic correlation function of: The systematic errors between the three-multipole and three-wedge methods are similar and the errors reported are always the largest of the two possibilities. For the analysis of the final eBOSS quasar sample, further work on improving the fidelity of the OuterRim-based mocks and understanding the difference in the bias models is needed. In particular, Vlah, Castorina White ( 2016 ) extended the CLPT-GS formalism to take into account contributions from effective field theory and additional bias terms. They showed that the effects of the biasing scheme are as important as higher order corrections to the theoretical predictions. Therefore, it would be interesting to see how this model performs for the analysis of the final eBOSS sample. Improvements in the model to account for the shape of the redshift error distribution would also be valuable. 5 ANALYSIS This section reviews the weighting scheme applied to the data to treat the potential systematic effects. We denote the total weighting scheme by , where the subscript specifies the different methods to compute the total weight. With this notation, the total weighting scheme used for the DR14 quasar BAO analysis (Ata et al. 2017 ) is: The first term, FKP = 1/(1 + n ( z ) P 0 ), is the FKP weight (Feldman, Kaiser Peacock 1994 ) that corrects for the variations of the observed quasar density n ( z ) across the redshift range and also depends on the amplitude of the power spectrum at the scale at which the FKP weights optimize the measurements (here we choose k = 0.14 h Mpc which is the typical scale at which the BAO signal is optimally detected which gives P 0 = 6 × 10 3 h −3 Mpc 3 ). The second term, photo , is a photometry weight which corrects for the variation of the depth across the survey; cp , is a weight that accounts for the quasar targets that could not be measured due to fibre collision; and noz is a weight that addresses for the number of confirmed quasars for which a secure redshift could not be determined. We will show that the use of the redshift efficiency, ε( x, y ), across the focal plane as a weight, focal = 1/ε( x, y ) is more appropriate than noz . We adopt the following definition of the total weight : Each quasar in the DR14 catalogue is thus weighted by to correct for any spurious variation of the quasar densities and to provide a more isotropic selection. For the random catalogue, we apply the FKP weight alone as it corresponds to a Poisson sampling which should not be affected by inhomogeneities in the selection. In tests defined throughout the following subsections, using the ability to test against unbiased samples, we will demonstrate that this new weight reduces systematic effects on the quadrupole by a factor of three. Furthermore, the region close to μ = 1 is responsible for the remaining systematic shift, and we propose a method to take this into account. The fits are performed with the CLPT-GS model.