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Using data from the SAMI Galaxy Survey, we investigate the correlationbetween the projected stellar kinematic spin vector of 1397 SAMI galaxies andthe line-of-sight motion of their neighbouring galaxies. We calculate theluminosity-weighted mean velocity difference between SAMI galaxies and theirneighbours in the direction perpendicular to the SAMI galaxies angular momentumaxes. The luminosity-weighted mean velocity offsets between SAMI andneighbours, which indicates the signal of coherence between the rotation of theSAMI 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 thatthe average velocity offsets increase for neighbours out to 2 Mpc. However, thevelocities are consistent with zero or negative for neighbours outside 3 Mpc.The negative signals for neighbours at distance around 10 Mpc are alsosignificant at $\sim 2$ $\sigma$ level, which indicate that the positivesignals within 2 Mpc might come from the variance of large-scale structure. Wealso calculate average velocities of different subsamples, including galaxiesin different regions of the sky, galaxies with different stellar masses, galaxytype, $\lambda_{Re}$ and inclination. Although low-mass, high-mass, early-typeand low-spin galaxies subsamples show 2 - 3 $\sigma$ signal of coherence forthe neighbours within 2 Mpc, the results for different inclination subsamplesand large-scale results suggest that the $\sim 2 \sigma$ signals might resultfrom coincidental scatter or variance of large-scale structure. Overall, themodest evidence of coherence signals for neighbouring galaxies within 2 Mpcneeds to be confirmed by larger samples of observations and simulation studies.

The SAMI Galaxy Survey: The relationship between galaxy rotation and the motion of neighbours