  Globular clusters (GCs) are among the oldest stellar systems in the universe.
As such, GCs population are valuable fossil tracers of galaxy formation and
interaction history. We use the multi-band wide-field images obtained with the
VST to study the properties of the GC population in an interacting pair of
galaxies. We derived ugri photometry over $1.5x1.5deg^2$ centred on the galaxy
group composed by two elliptical galaxies: NGC3640 and its fainter companion
NGC3641. We studied the GC system properties from both the ugri and gri matched
catalogs GC candidates were identified based on a combination of photometric
properties (colors, magnitudes) and morphometric criteria (concentration index,
elongation, FWHM), using sources with well-defined classifications from
spectroscopic or imaging data available in the literature and numerical
simulations as references. The selection criteria were also applied to empty
fields to determine a statistical background correction for the number of
identified GC candidates. The 2D density maps of GCs appear to align with the
diffuse light patches resulting from merging events of the galaxies. The
highest density peak of GCs is observed to be on NGC3641 rather than NGC3640,
despite the latter being the more massive galaxy. The azimuthal averaged radial
density profiles in both galaxies reveal that the GC population extends beyond
the galaxy light profile and indicate the likely presence of an intra-group GC
component. A color bimodality in (u-r) and (g-i) is observed for NGC3641,
whereas NGC3640 shows a broad unimodal distribution. Analysis of the GC
Luminosity Function indicates that both galaxies are roughly located at the
same distance (~27Mpc). We provide an estimate of the total number of GCs, and
determine the specific frequency for NGC3640, $S_N =2.0\pm0.6$, which aligns
with expectations, while for NGC3641 we find a large $S_N=4.5\pm1.6$.
