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Wide-field $u'g'r'i'z'$ Dark Energy Camera observations centred on the giantelliptical galaxy NGC5128 covering $\sim21deg^2$ are used to compile a newcatalogue of $\sim3200$ globular clusters (GCs). We report 2404 new candidates,including the vast majority within $\sim140$kpc of NGC5128. We find evidencefor a transition at a galactocentric radius of $R_{\rm gc}\approx55$kpc fromGCs intrinsic to NGC5128 to those likely to have been accreted from dwarfgalaxies or that may transition to the intra-group medium of the Centaurus Agalaxy group. We fit power-law surface number density profiles of the form$\Sigma_{N, R_{\rm gc}}\propto R_{\rm gc}^\Gamma$ and find that inside thetransition radius, the red GCs are more centrally concentrated than the blue,with $\Gamma_{\rm inner,red}\approx-1.78$ and $\Gamma_{\rminner,blue}\approx-1.40$. Outside this region both profiles flatten, moredramatically for the red GCs ($\Gamma_{\rm outer,red}\approx-0.33$) compared tothe blue ($\Gamma_{\rm outer,blue}\approx-0.61$), although the former is morelikely to suffer contamination by background sources. The median$(g'\!-\!z')_0\!=\!1.27$mag colour of the inner red population is consistentwith arising from the amalgamation of two giant galaxies each less luminousthan present-day NGC5128. Both in- and out-ward of the transition radius, wefind the fraction of blue GCs to dominate over the red GCs, indicating a livelyhistory of minor-mergers. Assuming the blue GCs to originate primarily in dwarfgalaxies, we model the population required to explain them, while remainingconsistent with NGC5128's present-day spheroid luminosity. We find that severaldozen dwarfs of luminosities $L_{dw,V}\simeq10^{6-9.3}L_{V,\odot}$, following aSchechter luminosity function with a faint-end slope of$-1.50\leq\alpha\leq-1.25$ is favoured, many of which may have already beendisrupted in NGC5128's tidal field.

The Survey of Centaurus A's Baryonic Structures (SCABS). II. The Extended Globular Cluster System of NGC5128 and its Nearby Environment