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Fig. 11


Projected surface density distribution of all selected globular clusters as function of their galactocentric distance to NGC 1399. The red line shows the best-fit power law to the red globular clusters with an exponent of n = −1.74 whereas the blue line shows the best-fit power law to the blue GC population, which has a more shallow slope of n = −1.12. The two short horizontal lines show the respective background levels used for the statistical correction of our signal. The dashed black lines show the radial interval to which we restricted our fit.

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