power-law for the high-mass end, $0.5<M/\Msun\le m_{TO}$, with a variable slope $x$;

-   and a power-law for the mass bins of the dark-remnants where to put all the evolved stars with mass above the TO mass, $m_{TO}<M/\Msun\le 8.0$: essentially white dwarfs. Here we adopted a fixed slope of 1.35, The mass of the WDs were set according to the initial-final mass relation of [@W90].

To build the mass segregation curves we varied the MF slope $x$ (the only variable parameter of the models) of the high-mass end stars in the range $-1.0\div1.35$, finding for each slope the model best fitting the radial density profile of the cluster. Then we calculated the radial variation of $x$ for the best-fit models in the same mass range of the observed stars: $0.5<M/M_{\odot}<m_{TO}$. The radial variations of $x$ are compared with the observed MFs in Figure \[M55slx\]. The mass function slopes are shown at the right end of each curve. This plot is similar to those presented in [@Pryor86], and allows one to obtain the value of the global mass function of the cluster. The three observed points follow fairly well the theoretical curves. Also the high-mass MF slope value of [@Mand96] (open circle 