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Galactic star clusters are known to harbour a significant amount of binarystars, yet their role in the dynamical evolution of the cluster as a whole isnot comprehensively understood. We investigated the influence of binary starson the total mass estimate for the case of the moderately populated Galacticstar cluster NGC 225. The analysis of multi-epoch radial velocities of the 29brightest cluster members, obtained over two observational campaigns, in1990-1991 and in 2019-2020, yields a value of binary fraction of $\alpha =0.52$(15 stars out of 29). Using theoretical isochrones and Monte Carlo simulationswe found that the cluster mass increases at least 1.23 times when binaries areproperly taken into account. By combining Gaia EDR3 photometric data with ourspectroscopic observations, we derived estimates of NGC 225 fundamentalparameters as follows: mean radial velocity $<V_r> = -9.8 \pm 0.7$ km s$^{-1}$,$\log(\tau)$=8.0-8.2 dex, distance $ D = 676 \pm 22$ pc, and colour excess$E(B-V) = 0.29 \pm 0.01$ mag.

The young Galactic cluster NGC 225: binary stars content and total mass estimate