  In this work we perform the photometric analysis of the globular cluster
system (GCS) of the giant elliptical NGC4696, which is the brightest member of
Centaurus, a rich and dynamically young galaxy cluster. We obtained deep
Magellan 6.5 m/MegaCam (g', r', i') photometry, with which we identified a
sample of 3818 stellar clusters around NGC4696 that were analyzed in the
context of possible interactions and its assembly history. After carefully
modeling and subtracting the galaxy light, we used selection criteria based on
the shape, colors, and magnitudes to identify GC candidates. We find a number
of features that indicate a disturbed GCS that points toward a complex
evolution with other neighboring members of Centaurus. Formally, two
subpopulations could be found at (g'-i')_0 = 0.763 $\pm$ 0.004 and
(g'-i')_0=1.012 $\pm$ 0.004. Moreover, the color distribution does not show the
presence of a significant blue tilt, but it presents a trend with the radius,
where at small galactocentric distances a unimodal distribution is preferable
to a bimodal one, suggesting the presence of an intermediate GC population.
Besides the color distribution, the metallicity distribution also shows a
bimodal trend, with peaks at [Fe/H]=-1.363 $\pm$ 0.010 and [Fe/H]=-0.488 $\pm$
0.012. The radial density profiles show different slopes for the blue and red
populations and the azimuthal distributions are well fitted by an asymmetrical
sinusoidal function, with peaks projecting toward two nearby galaxies, NGC4696B
and NGC4709, indicating past interactions among these three galaxies. Finally,
we derived a GC specific frequency of S_N=6.8 $\pm$ 0.9, in good agreement with
the values obtained for other giant ellipticals and with previously estimated
S_N of NGC4696. All these results point toward a complex GCS, strongly
influenced by the interaction history of NGC4696 with the other galaxies of the
Centaurus cluster.
