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The activity of central supermassive black holes might affect the alignmentof galaxy spin axes with respect to the closest cosmic filaments. We exploitthe SAMI Galaxy Survey to study possible relations between black hole activityand the spin-filament alignments of stars and ionised gas separately. Toexplore the impact of instantaneous black hole activity, active galaxies areselected according to emission-line diagnostics. Central stellar velocitydispersion ($\sigma_c$) is used as a proxy for black hole mass and itsintegrated activity. We find evidence for the gas spin-filament alignments tobe influenced by AGN, with Seyfert galaxies showing a stronger perpendicularalignment at fixed bulge mass with respect to galaxies where ionisation isconsequence of low-ionizaition nuclear emission-line regions (LINERs) or oldstellar populations (retired galaxies). On the other hand, the greaterperpendicular tendency for the stellar spin-filament alignments of high-bulgemass galaxies is dominated by retired galaxies. Stellar alignments show astronger correlation with $\sigma_c$ compared to the gas alignments. We confirmthat bulge mass ($M_{bulge}$) is the primary parameter of correlation for bothstellar and gas spin-filament alignments (with no residual dependency left for$\sigma_c$), while $\sigma_c$ is the most important property for secular starformation quenching (with no residual dependency left for $M_{bulge}$). Thesefindings indicate that $M_{bulge}$ and $\sigma_c$ are the most predictiveparameters of two different galaxy evolution processes, suggesting mergerstrigger spin-filament alignment flips and integrated black hole activity drivesstar formation quenching.

The SAMI Galaxy Survey: impact of black hole activity on galaxy spin-filament alignments