All Figures

	Figure 1: Negative image of the cluster NGC 2298 through the F606W band. The field spans on a side. The circles marked on the frame define the six annuli in which we have divided our photometry, as explained in Sect. 3.
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In the text

	Figure 2: Colour-magnitude diagram of an area of around the centre of NGC 2298.
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In the text

	Figure 3: Main sequence ridge line of NGC 2298 (filled circles) compared with the theoretical isochrones of Baraffe et al. (1997; dashed line) for an age of 10 Gyr and metallicity [M/H]=-1.5, in the magnitude system of the ACS (see text).
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In the text

Figure 4: The circles are the LFs of the six rings, after correction for photometric incompleteness (see Table 2). The actual measurements from Table 3 are shifted vertically by an arbitrary amount to increase readability. The geometric average radius of each ring is indicated in arcmin to the left of each curve. The theoretical LFs that best fit the data are shown as solid lines. The index of their corresponding power-law MF is, from bottom to top, and -0.1. A positive index means that the number of stars decreases with mass. All but the innermost LF reach down to 0.2 . The dashed line is the LF measured near the half-mass radius of NGC 6397 by De Marchi et al. (2000), with arbitrary vertical normalisation.

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In the text

	Figure 5: The LFs of Fig. 4 (circles) are compared with those predicted by our multi-mass Michie-King model at various radii inside the cluster (dashed lines), for a GMF with index . The expected radial variation of the LF is fully consistent with the observations.
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In the text

	Figure 6: The surface brightness profile of NGC 2298 (crosses, from Trager et al. 1995) is well reproduced by our dynamical model (solid line). The observations are normalised to the central value of the best fitting profile as given by Trager et al. (1995).
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In the text