  The activity of central supermassive black holes might affect the alignment
of galaxy spin axes with respect to the closest cosmic filaments. We exploit
the SAMI Galaxy Survey to study possible relations between black hole activity
and the spin-filament alignments of stars and ionised gas separately. To
explore the impact of instantaneous black hole activity, active galaxies are
selected according to emission-line diagnostics. Central stellar velocity
dispersion ($\sigma_c$) is used as a proxy for black hole mass and its
integrated activity. We find evidence for the gas spin-filament alignments to
be influenced by AGN, with Seyfert galaxies showing a stronger perpendicular
alignment at fixed bulge mass with respect to galaxies where ionisation is
consequence of low-ionizaition nuclear emission-line regions (LINERs) or old
stellar populations (retired galaxies). On the other hand, the greater
perpendicular tendency for the stellar spin-filament alignments of high-bulge
mass galaxies is dominated by retired galaxies. Stellar alignments show a
stronger correlation with $\sigma_c$ compared to the gas alignments. We confirm
that bulge mass ($M_{bulge}$) is the primary parameter of correlation for both
stellar and gas spin-filament alignments (with no residual dependency left for
$\sigma_c$), while $\sigma_c$ is the most important property for secular star
formation quenching (with no residual dependency left for $M_{bulge}$). These
findings indicate that $M_{bulge}$ and $\sigma_c$ are the most predictive
parameters of two different galaxy evolution processes, suggesting mergers
trigger spin-filament alignment flips and integrated black hole activity drives
star formation quenching.
