VEGAS-SSS: Tracing globular cluster populations in the interacting NGC3640 galaxy group

Globular clusters (GCs) are among the oldest stellar systems in the universe. As such, GC populations are valuable fossil tracers of galaxy formation and interaction history. This paper is part of the VEGAS-SSS series, which focuses on studying the properties of small stellar systems (SSSs) in and around bright galaxies. We used the multiband 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 $1.5 1.5$ sq. degrees centered on the galaxy group composed of two elliptical galaxies: NGC\,3640 and its fainter companion NGC\,3641. 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 and magnitudes) and morphometric criteria (concentration index, elongation, FWHM, etc.), 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 the merging events of the galaxies. The highest density peak of GCs is observed to be on NGC\,3641 rather than NGC\,3640, 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 this indicates the likely presence of an intra-group GC component. A color bimodality in r)$ and $(g i)$ is observed for NGC\,3641, whereas NGC\,3640 shows a broad unimodal distribution. Analysis of the GC luminosity function indicates that both galaxies are roughly located at the same distance (sim 27 Mpc). We provide an estimate of the total number of GCs, and determine the specific frequency for NGC\,3640 N $ =2.0pm 0.6, which aligns with expectations, while for NGC\,3641 we find a large N $ = 4.5pm 1.6.