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It is now recognised that the traditional method of calculating the LSRfails. We find an improved estimate of the LSR by making use of the larger andmore accurate database provided by XHIP and repeating our preferred analysisfrom Francis & Anderson (2009a). We confirm an unexpected high value of $U_0$by calculating the mean for stars with orbits sufficiently inclined to theGalactic plane that they do not participate in bulk streaming motions. Our bestestimate of the solar motion with respect to the LSR $(U_0, V_0, W_0) = (14.1\pm 1.1, 14.6 \pm 0.4, 6.9 \pm 0.1)$ km\ s$^{-1}$.

The local standard of rest and the well in the velocity distribution