Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555.

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We note here that, due to the $\sim$ $20\hbox{$^{\prime\prime}$ }$ gap between the two detectors of the ACS/WFC and in light of the dithering pattern used for these observations, the cluster centre and the regions to the right and to the left of it in the images do not have the same photometric depth as the other parts of the frames. We have deliberately avoided these regions and, therefore, no photometry exists for certain sections of the rings. Therefore, the number of objects detected in each ring does not necessarily correspond to the radial density profile.

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...2000)

Note that, since NGC 2298 and NGC 6397 have a very similar metallicity, the two GMFs were determined by using the same M-L relationship. Therefore, any differences in the resulting GMFs reflect the physical properties of the clusters and are rather insensitive to the uncertainties in the theoretical M-L models.

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