Fig. 21
Upper panel: MS dispersion as a function of mF814W magnitude for NGC 2298. Circles and triangles correspond to real and artificial stars, respectively. The corresponding best fitting 4th order polynomials are represented by dotted and dashed lines. Lower panels: comparison of the observed CMD of NGC 2298 (left) and the CMDs of artificial stars before (middle) and after (right) the application of color spread.
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