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Using the cosmological hydrodynamics simulation Horizon-AGN, we investigatethe spatial distribution of satellite galaxies relative to their centralcounterpart in the redshift range between 0.3 and 0.8. We find that, onaverage, these satellites tend to be located on the galactic plane of thecentral object. This effect is detected for central galaxies with a stellarmass larger than 10^10 solar masses and found to be strongest for red passivegalaxies, while blue galaxies exhibit a weaker trend. For galaxies with a minoraxis parallel to the direction of the nearest filament, we find that thecoplanarity is stronger in the vicinity of the central galaxy, and decreaseswhen moving towards the outskirts of the host halo. By contrast, the spatialdistribution of satellite galaxies relative to their closest filament followsthe opposite trend: their tendency to align with them dominates at largedistances from the central galaxy, and fades away in its vicinity. Relying onmock catalogs of galaxies in that redshift range, we show that massive redcentrals with a spin perpendicular to their filament also have corotatingsatellites well aligned with both the galactic plane and the filament. On theother hand, lower-mass blue centrals with a spin parallel to their filamenthave satellites flowing straight along this filament, and hence orthogonally totheir galactic plane. The orbit of these satellites is then progressively benttowards a better alignment with the galactic plane as they penetrate thecentral region of their host halo. The kinematics previously described areconsistent with satellite infall and spin build-up via quasi-polar flows,followed by a re-orientation of the spin of massive red galaxies throughmergers.

Caught in the rhythm: how satellites settle into a plane around their central galaxy