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Cluster number counts will be a key cosmological probe in the next decadethanks to the Euclid satellite mission. For this purpose, cluster detectionalgorithm performance, which are sensitive to the spatial distribution of thecluster galaxy members and their luminosity function, need to be accuratelycharacterized. Using The Three Hundred hydrodynamical and dark matter onlysimulations we study a complete sample of massive clusters beyond 7 (5)$\times$ 10$^{14}$ M$_{\odot}$ at redshift 0 (1) on a $(1.48 \ \mathrm{Gpc})^3$volume. We find that the mass resolution of the current hydrodynamicalsimulations (1.5 $\times$ 10$^9$ M$_{\odot}$) is not enough to characterize theluminosity function of the sample in the perspective of Euclid data.Nevertheless, these simulations are still useful to characterize the spatialdistribution of the cluster substructures assuming a common relative massthreshold for the different flavours and resolutions. By comparing with thedark matter only version of these simulations, we demonstrate that baryonicphysics preserves significantly low mass subhalos (galaxies) as have also beenobserved in previous studies with less statistics. Furthermore, by comparingthe hydro simulations with higher resolution dark matter only simulations ofthe same objects and taking the same limit in subhalo mass we findsignificantly more cuspy galaxy density profiles towards the center of theclusters, where the low mass substructures would tend to concentrate. Weconclude that using dark matter only simulation may lead to some biases on thespatial distribution and density of galaxy cluster members. Based on thepreliminary analysis of few high resolution hydro simulations we conclude thata mass resolution of 1.8 $\times$ 10$^8$ h$^{-1}$ M$_{\odot}$ will be neededfor The Three Hundred simulations to approach the expected magnitude limits forthe Euclid survey.

The Three Hundred : contrasting clusters galaxy density in hydrodynamical and dark matter simulations