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tokens: SDSS DR7 and DR13 galaxy samples in two redshift bins for the different models of the LF described in the text. The quoted errors represent marginalized 68percent confidence intervals. Considering total bulk flow amplitudes, the DR13 estimates are generally smaller than the DR7 ones. Averaging the results over the different LF models yields values of and 48595 in units of km s 1 for the low- and high-redshift bin, respectively. In the high- z bin, the flow amplitudes are reduced by about 50200kms 1 compared to DR7, where the most significant changes appear for the Schechter model of the LF. The bulk flow components found from estimators using different LF models are in reasonable agreement, typically consistent within the quoted uncertainties. Assuming the results based on the hybrid model, the estimated bulk flows from DR13 are pointing towards ( l , b ) (315, 17)(52, 15) and (304, 22)(14, 11) for the first and second redshift bin, respectively. Similar directions are obtained for the other estimators. To better assess these measurements, we repeated the analysis for the 269 mock galaxy catalogues introduced in Section 3.2 . In contrast to the study presented in Feix etal. ( 2014 ), these mocks do not account for the photometric tilt of the SDSS DR7 calibration that severely contaminates bulk flows measured through the luminosity approach. The results based on our mocks suggest that the individual flow components obtained with our methods are not statistically independent, but subject to correlations at the level of 0.10.3. If the joint distribution of bulk flow components is approximately given by a multivariate Gaussian with covariance matrix B , the quadratic form should follow a 2 -distribution with k 3 degrees of freedom. To test the validity of this assumption, we computed directly from the SDSS mocks. For the Schechter LF model, the resulting distributions, plotted as histograms in Fig. 2 , are indeed well matched by the 2 -distribution (solid curves). Adopting the other models of the LF yields very similar results. Using the estimate of B from the mock catalogues, we may therefore assign probabilities to the bulk flow measurements listed in Table 1 . As customary, we express these in terms of confidence limits based on normally distributed data. Figure 2. Distribution of the quadratic form in two redshift bins derived from the SDSS mock catalogues, assuming the Schechter model of the LF: the histograms represent the observed (normalized) distribution and solid lines correspond to the 2 -distribution with k 3 degrees of freedom. The corresponding event levels (in units of the standard deviation ) for the inferred bulk flow amplitudes are presented in Table 2 . Compared to the DR7 results, the probability estimates of the DR13 measurements are on average considerably larger, and thus consistent with an improved photometric calibration. The most prominent change is found in the high- z bin for the Schechter model of the LF, where the