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We study the alignments of galaxy spin axes with respect to cosmic webfilaments as a function of various properties of the galaxies and theirconstituent bulges and discs. We exploit the SAMI Galaxy Survey to identify 3Dspin axes from spatially-resolved stellar kinematics and to decompose thegalaxy into the kinematic bulge and disc components. The GAMA survey is used toreconstruct the cosmic filaments. The mass of the bulge, defined as the productof stellar mass and bulge-to-total flux ratio M_bulge=M_star x (B/T), is theprimary parameter of correlation with spin-filament alignments: galaxies withlower bulge masses tend to have their spins parallel to the closest filament,while galaxies with higher bulge masses are more perpendicularly aligned.M_star and B/T separately show correlations, but they do not fully unravelspin-filament alignments. Other galaxy properties, such as visual morphology,stellar age, star formation activity, kinematic parameters and localenvironment, are secondary tracers. Focusing on S0 galaxies, we findpreferentially perpendicular alignments, with the signal dominated by high-massS0 galaxies. Studying bulge and disc spin-filament alignments separatelyreveals additional information about the formation pathways of thecorresponding galaxies: bulges tend to have more perpendicular alignments,while discs show different tendencies according to their kinematic features andthe mass of the associated bulge. The observed correlation between the flippingof spin-filament alignments and the growth of the bulge can be explained bymergers, which drive both alignment flips and bulge formation.

The SAMI Galaxy Survey: flipping of the spin-filament alignment correlates most strongly with growth of the bulge