not fitted their data directly but made only a comparison with a plot of King models.

\[extrat\]

The density profile for different stellar masses.
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Having verified the compatibility of our density profile with previously published ones, we have extracted surface density profiles for different magnitude ranges corresponding to different stellar masses. The adopted magnitude intervals have been chosen to have a significant number of stars in each bin. We used logarithmic radial binning that allows a better sampling of the stars in the outer part of the cluster. In order to lower the noise in the outer part of the profile, we have smoothed the profiles with a median static filter of fixed width of 3 points. We verified that the filtering procedure did not introduce spurious radial gradients in the density profiles. The mean masses in each magnitude bin adopted for the profiles, as obtained from the isochrone by [@VDB85] ( also Section \[Sm55mf\]), are:

[cc]{} $V$ & $<m>$\
$<18$ & 0.79\
$18-19$ & 0.77\
$19-20$ & 0.71\
$20-20.9$& 0.63\

The relative profiles, without subtraction of the background stars, are shown in Figure \[profconf\] and \[extrat\]. The arrows in both figures indicate $r_c$, $2~r_c$ and $r_t$.

The profiles 