  We investigate the 3D spin alignment of galaxies with respect to the
large-scale filaments using the MaNGA survey. The cosmic web is reconstructed
from the Sloan Digital Sky Survey using Disperse and the 3D spins of MaNGA
galaxies are estimated using the thin disk approximation with integral field
spectroscopy kinematics. Late-type spiral galaxies are found to have their
spins parallel to the closest filament's axis. The alignment signal is found to
be dominated by low-mass spirals. Spins of S0-type galaxies tend to be oriented
preferentially in perpendicular direction with respect to the filament's axis.
This orthogonal orientation is found to be dominated by S0s that show a notable
misalignment between their kinematic components of stellar and ionised gas
velocity fields and/or by low mass S0s with lower rotation support compared to
their high mass counterparts. Qualitatively similar results are obtained when
splitting galaxies based on the degree of ordered stellar rotation, such that
galaxies with high spin magnitude have their spin aligned, and those with low
spin magnitude in perpendicular direction to the filaments. In the context of
conditional tidal torque theory, these findings suggest that galaxies' spins
retain memory of their larger-scale environment. In agreement with measurements
from hydrodynamical cosmological simulations, the measured signal at low
redshift is weak, yet statistically significant. The dependence of the
spin-filament orientation of galaxies on their stellar mass, morphology and
kinematics highlights the importance of sample selection to detect the signal.
