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We perform a detailed study of the Globular Cluster (GC) system in the galaxyNGC5866 based on F435W, F555W, and F625W (~ B, V, and R) HST Advanced Camerafor Surveys images.  Adopting color, size and shape selection criteria, the final list of GCcandidates comprises 109 objects, with small estimated contamination frombackground galaxies, and foreground stars.  The color distribution of the final GC sample has a bimodal form. Adoptingcolor to metallicity transformations derived from the Teramo--SPoT simplestellar population model, we estimate a metallicity [Fe/H]~ -1.5, and -0.6 dexfor the blue and red peaks, respectively. A similar result is found if theempirical color-metallicity relations derived from Galactic GCs data are used.  The two subpopulations show some of the features commonly observed in the GCsystem of other galaxies, like a ``blue tilt'', higher central concentrationsof the red subsystem, and larger half--light radii at larger galactocentricdistances. However, we do not find evidence of a substantial difference betweenthe average sizes of red and blue clusters.  Our analysis of the GC Luminosity Function indicates a V-band Turn-OverMagnitude V$_0^{TOM}$=23.46+-0.06, or M$_{V,0}^{TOM}\sim-7.29 +- 0.10$ mag,using the distance modulus derived from the average of SBF and the PNLFdistances. The absolute Turn-Over Magnitude obtained agrees well withcalibrations from literature. The specific frequency is measured to be $S_N=1.4+- 0.3$, typical for galaxies of this type.

The globular cluster system in NGC5866: optical observations from HST Advanced Camera for Surveys