It is now recognised that the traditional method of calculating the LSR fails .
We find an improved estimate of the LSR by making use of the larger and more accurate database provided by XHIP and repeating our preferred analysis from Francis & Anderson ( 2009a ) .
We confirm an unexpected high value of U _ { 0 } by calculating the mean for stars with orbits sufficiently inclined to the Galactic plane that they do not participate in bulk streaming motions .
Our best estimate 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 } .