  The dynamical evolution of globular clusters is theoretically described by a
series of well known events typical of N-body systems. Still, the
identification of observational signatures able to empirically describe the
stage of dynamical evolution of a stellar system of the density typical of a
globular cluster, represents a challenge. In this paper we study the dynamical
age of the globular clusters Rup 106 and IC 4499. To this aim, we study the
radial distribution of the Blue Straggler Stars via the A+ parameter and of the
slope of the Main Sequence Mass Function. Both tracers show that Rup 106 and IC
4499 are dynamically young clusters where dynamical friction has just started
to segregate massive stars towards the clusters' centre. In fact, we observe
that the Blue Straggler stars are more centrally concentrated in both clusters
than the reference population. On the same line, we find that in both cases the
slope of the mass function significantly decreases as a function of the
cluster-centric distances. This result provides additional support for the use
of the the radial distribution of the blue stragglers as a powerful
observationally convenient indicator of the cluster dynamical age.
