  Stars evolving around a supermassive black hole see their orbital
orientations diffuse efficiently, a process called "vector resonant
relaxation". In particular, stars within the same disc, i.e. neighbors in
orientations, will slowly diffuse away from one another through this stochastic
process. We use jointly (i) detailed kinetic predictions for the efficiency of
this dilution and (ii) the recent observation of a stellar disc around SgrA*,
the supermassive black hole at the centre of the Milky-Way, to constrain
SgrA*'s unobserved stellar cluster. Notably, we investigate quantitatively the
impact of a population of intermediate mass black holes on the survivability of
the stellar disc.
