  The effect of angular momentum on galaxy formation and evolution has been
studied for several decades. Our recent two papers using IllustrisTNG-100
simulation have revealed the acquisition path of the angular momentum from
large-scale environment (satellites within hundreds of kpc) through the
circum-galactic medium (CGM) to the stellar discs, putting forward the
co-rotation scenario across the three distance scales. In real observations,
although the rotation signature for the CGM and environmental three-dimensional
(3d) angular momentum are difficult to obtain, line-of-sight kinematics of
group member galaxies and stellar disc kinematics of central galaxies are
available utilizing existing group catalogue data and integral field unit (IFU)
data. In this paper, we use (1) the group catalogue of SDSS DR7 and MaNGA IFU
stellar kinematic maps and (2) the group catalogue of GAMA DR4 data and SAMI
IFU stellar kinematic maps, to test if the prediction above can be seen in real
data. We found the co-rotation pattern between stellar discs and satellites can
be concluded with 99.7 percent confidence level ($\sim 3\sigma$) when combining
the two datasets. And the random tests show that the signal can be scarcely
drawn from random distribution.
