  Using data from the SAMI Galaxy Survey, we investigate the correlation
between the projected stellar kinematic spin vector of 1397 SAMI galaxies and
the line-of-sight motion of their neighbouring galaxies. We calculate the
luminosity-weighted mean velocity difference between SAMI galaxies and their
neighbours in the direction perpendicular to the SAMI galaxies angular momentum
axes. The luminosity-weighted mean velocity offsets between SAMI and
neighbours, which indicates the signal of coherence between the rotation of the
SAMI galaxies and the motion of neighbours, is 9.0 $\pm$ 5.4 km s$^{-1}$ (1.7
$\sigma$) for neighbours within 1 Mpc. In a large-scale analysis, we find that
the average velocity offsets increase for neighbours out to 2 Mpc. However, the
velocities are consistent with zero or negative for neighbours outside 3 Mpc.
The negative signals for neighbours at distance around 10 Mpc are also
significant at $\sim 2$ $\sigma$ level, which indicate that the positive
signals within 2 Mpc might come from the variance of large-scale structure. We
also calculate average velocities of different subsamples, including galaxies
in different regions of the sky, galaxies with different stellar masses, galaxy
type, $\lambda_{Re}$ and inclination. Although low-mass, high-mass, early-type
and low-spin galaxies subsamples show 2 - 3 $\sigma$ signal of coherence for
the neighbours within 2 Mpc, the results for different inclination subsamples
and large-scale results suggest that the $\sim 2 \sigma$ signals might result
from coincidental scatter or variance of large-scale structure. Overall, the
modest evidence of coherence signals for neighbouring galaxies within 2 Mpc
needs to be confirmed by larger samples of observations and simulation studies.
