We use about 200,000 FGK type main-sequence stars from the LAMOST DR1 data to map the local stellar kinematics .
With the velocity de-projection technique , we are able to derive the averaged 3 dimensional velocity and velocity ellipsoids using only the line-of-sight velocity for the stars with various effective temperatures within 100 < |z| < 500 pc .
Using the mean velocities of the cool stars , we derive the solar motion of ( { U _ { \odot } } , { V _ { \odot } } , { W _ { \odot } } ) = ( 9.58 \pm 2.39 , 10.52 \pm 1.96 , 7.01 \pm 1.67 ) \mathrm { km s } ^ { -1 } with respect to the local standard of rest .
Moreover , we find that the stars with { T } _ { eff } > 6000 K show a net asymmetric motion of \sim 3 \mathrm { km s } ^ { -1 } in \langle W \rangle compared to the stars with { T } _ { eff } < 6000 K. And their azimuthal velocity increases when |z| increases .
This peculiar motion in the warmer stars is likely because they are young and not completely relaxed , although other reasons , such as the resonance induced by the central rotating bar or the spiral structures , and the perturbation of the merging dwarf galaxies , can not be ruled out .
The derived velocity dispersions and cross terms for the data are approximately consistent with previous studies .
We also find that the vertical gradients of \sigma _ { U } and \sigma _ { V } are larger than that of \sigma _ { W } .
And the vertical gradient of \sigma _ { U } shows clear correlation with { T } _ { eff } , while the other two do not .
Finally , our sample shows vertex deviation of about 11 ^ { \circ } , at 300 < |z| < 500 pc , but roughly zero at 100 < |z| < 300 pc .