Context : Luminous elliptical galaxies generally display a rich star cluster system , whose properties provide strong constraints on the physics of galaxy formation and evolution . Star cluster system studies , however , concentrate on galaxies located in nearby or rich galaxy clusters . Aims : We acquired deep B and I images of NGC 1600 , a luminous elliptical in a galaxy group to study its star cluster system . The images were obtained with the Optical Imager at the Southern Telescope for Astrophysical Research for an exposure time of 1.66hr in each filter . Methods : The sample selection incompleteness was assessed as a function of magnitude and image background level . Source counts were measured for different elliptical annuli from the centre of NGC 1600 , background subtracted , and fitted with a Gaussian function . Colour distributions were derived as a function of galactocentric distance for sources measured successfully in both filters . Typical ages and metallicities were estimated based on single stellar population models . Results : A clear excess of point sources around NGC 1600 was found in relation to the nearby field . The source counts were consistent with a Gaussian distribution typical of other luminous ellipticals . The luminosity function fits provided an estimate of the density of clusters at the different annuli that could be integrated in solid angle , resulting in an estimated total population of N _ { GC } \simeq 2850 star clusters . This yielded a specific frequency of S _ { N } \simeq 1.6 . The colour distributions show a hint of bimodality , especially at \simeq 20 kpc from the centre . Clusters in this region may be associated with a ring or shell perturbation . Finally , the star cluster candidates were cross-correlated to discrete X-ray sources and a coincidence rate of \simeq 40 \% was found . These are likely to be globular clusters harboring low-mass X-ray binaries . Conclusions :