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We investigate the rate of orbital orientation dilution of young stellarclusters in the vicinity of supermassive black holes. Within the framework ofvector resonant relaxation, we predict the time evolution of the two-pointcorrelation function of the stellar orbital plane orientations as a function oftheir initial angular separation and diversity in orbital parameters(semi-major axis, eccentricity). As expected, the larger the spread in initialorientations and orbital parameters, the more efficient the dilution of a givenset of co-eval stars, with a characteristic timescale set up by the coherencetime of the background potential fluctuations. A Markovian prescription whichmatches numerical simulations allows us to efficiently probe the underlyingkinematic properties of the unresolved nucleus when requesting consistency witha given dilution efficiency, imposed by the observed stellar disc within theone arcsecond of Sgr A*. As a proof of concept, we compute maps of constantdilution times as a function of the semi major axis cusp index and fraction ofintermediate mass black holes in the old background stellar cluster. Thiscomputation suggests that vector resonant relaxation should prove useful inthis context since it impacts orientations on timescales comparable to thestars' age.

Young stellar cluster dilution near supermassive black holes: the impact of Vector Resonant Relaxation on neighbour separation