We present Integral Field Unit ( IFU ) spectroscopy of four brightest cluster galaxies ( BCGs ) at z \sim 0.1 .
Three of the BCGs have close companions within a projected radius of 20 kpc and one has no companion within that radius .
We calculate the dynamical masses of the BCGs and their companions to be 1.4 \times 10 ^ { 11 } < M _ { dyn } ( M _ { \odot } ) < 1.5 \times 10 ^ { 12 } .
We estimate the probability that the companions of the BCGs are bound using the observed masses and velocity offsets .
We show that the lowest mass companion ( 1:4 ) is not bound while the two nearly equal mass ( 1:1.45 and 1:1.25 ) companions are likely to merge with their host BCGs in 0.35 Gyr in major , dry mergers .
We conclude that some BCGs continue to grow from major merging even at z \sim 0 .
We analyse the stellar kinematics of these systems using the \lambda _ { R } parameter developed by the SAURON team .
This offers a new and unique means to measure the stellar angular momentum of BCGs and make a direct comparison to other early-type galaxies .
The BCGs and their companions have similar ellipticities to those of other early-type galaxies but are more massive .
We find that not all these massive galaxies have low \lambda _ { R _ { e } } as one might expect .
One of the four BCGs and the two massive companions are found to be fast-rotating galaxies with high angular momentum , thereby providing a new test for models of galaxy evolution and the formation of Intra-Cluster Light .