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Using Magellan/IMACS images covering a 1.2 x 1.2 sq. degree FOV with seeingof 0.4"-0.6", we have applied convolution techniques to analyse the lightdistribution of 364 confirmed globular cluster in the field of NGC 5128 and toobtain their structural parameters. Combining these parameters with existingWashington photometry from Harris et al. (2004), we are able to examine thesize difference between metal-poor (blue) and metal-rich (red) globularclusters. For the first time, this can be addressed on a sample of confirmedclusters that extends to galactocentric distances about 8 times the effectiveradius, R$_{eff}$, of the galaxy. Within 1 R$_{eff}$, red clusters are about30% smaller on average than blue clusters, in agreement with the vast majorityof extragalactic globular cluster systems studied. As the galactocentricdistance increases, however, this difference becomes negligible. Thus, ourresults indicate that the difference in the clusters' effective radii, r$_e$,could be explained purely by projection effects, with red clusters being morecentrally concentrated than blue ones and an intrinsic r$_e$--R$_{gc}$dependence, like the one observed for the Galaxy.

Sizes of Confirmed Globular Clusters in NGC 5128: A Wide-Field High-Resolution Study