shows that taking into account observing errors, M55 fairly fits into the relation given by [@Manu97], which is a refined version of the one found by [@DPC93]. A different conclusion has been reached by [@Mand96] using their uncorrected (for mass segregation) value for the MF of M55. As noted by the referee, M55 lies further from the average relation defined by the other clusters: of those with a similar abscissa ($0.0\pm0.2$), M55 is the one with the lowest value of $x$. It is not possible to identify the main source of this apparent enhanced mass-loss of M55 compared to the other clusters; a possible cause can be a orbit of the cluster that deeply penetrate into the bulge of the Galaxy. This cannot be confirmed until is performed a reliable measure of the proper motion of M55.

Radial density profile from star counts.\[M55rprof\]
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The CMD allows a unique way to obtain a reliable measure of the radial density profiles of GCs. In fact, the CMD allows us to sort out the stars belonging to the cluster, limiting the problems generated by the presence of the field stars. This also permits to extract radial profiles for distinct stellar masses.

We 