expected to be important [@n91], facilitating the comparison with cosmological models. The largest radius corresponds to the distance within which the data are used. Figure (\[fig:unb\]) shows the Galactic $x$ (blue dotted), $y$ (black solid), and $z$ (red dot-dashed) components of $\vace$ (top panel) and $\vmle$ (bottom) as a function of $r$. The magnitudes of $\vace$ and $\vmle$ versus radius are plotted, respectively, as the blue circles and plotted in figure (\[fig:btot\]). The $1\sigma$ errorbars in both figures are based on the 2200 mocks. The component $B_y$ is clearly the most significant. This is just a coincident and has no bearing on the statistical analysis of the results as one can always choose a coordinate system such that the bulk is along a given axis.The solid curve in this figure is the theoretical expectation of $\Lambda$CDM7 with but with $\sigma_8=0.85$ instead of the default $\sigma_8=0.8$. The theoretical curve is computed given the density power spectrum $p_{_\delta} (k,\Omega_m,\Omega_b,h,n_s)$ by $$\label{eq:sigv}
\sigma_v^2(r)=\frac{H_0^2 f^2}{2\pi^2}\int \dd k \; p_{_\delta} (k) W^2(k r)$$ where $f =\Omega_m^\gamma$ with a growth index $\gamma\approx 0.55$ for a flat Universe [@Lind05], and $W=W_{\rm TH}(k r){\rm exp}(-k^2R_s^2/2)$ with $W_{\rm TH}$ is the top-hat window function and the gaussian window takes 