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We present the first detection of mass dependent galactic spin alignmentswith local cosmic filaments with over 2 sigma confidence using IFS kinematics.The 3D network of cosmic filaments is reconstructed on Mpc scales across GAMAfields using the cosmic web extractor DisPerSe. We assign field galaxies fromthe SAMI survey to their nearest filament segment in 3D and estimate the degreeof alignment between SAMI galaxies kinematic spin axis and their nearestfilament in projection. Low-mass galaxies align their spin with their nearestfilament while higher mass counterparts are more likely to display anorthogonal orientation. The stellar transition mass from the first trend to thesecond is bracketed between log stellar masses 10.4 and 10.9, with hints of anincrease with filament scale. Consistent signals are found in the HorizonAGNcosmological hydrodynamic simulation. This supports a scenario of early angularmomentum build-up in vorticity rich quadrants around filaments at low stellarmass followed by progressive flip of spins orthogonal to the cosmic filamentsthrough mergers at high stellar mass. Conversely, we show that dark-matter onlysimulations post-processed with a semi-analytic model treatment of galaxyformation struggles to reproduce this alignment signal. This suggests that gasphysics is key in enhancing the galaxy-filament alignment.

The SAMI Galaxy Survey: First detection of a transition in spin orientation with respect to cosmic filaments in the stellar kinematics of galaxies