Mean peculiar velocity as a function of the angle between the galaxy-group and group-observer (θ) directions in the CF3S (points). Each panel corresponds to a different galaxy-group distance, as is indicated in the figure. The dashed line indicates the best linear fitting, the slope is associated to the infall amplitude (V_CF3S) and it is specified in each panel. The error bars correspond to the peculiar velocity dispersion. The gray shaded areas enclose the dispersion of mean peculiar velocity from the 25 biased mock catalogs. We note that the range of the y-axis in upper and lower panels is different.