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With the aim of tracing back the evolution of galaxies in nearby groups weuse smooth particle hydrodynamical (SPH) simulations with chemo-photometricimplementation. Here we focus on the evolution of the early-type members (Esand S0s, ETGs hereafter) in two groups, USGC U376 and LGG 225, both in the Leocloud. We use the near-UV (NUV)-optical rest-frame $NUV-r$ versus $M_r$ colormagnitude diagram to follow their evolution, from the blue cloud (BC) to thered sequence (RS), through the green valley (GV). ETGs brighter than $M_r=-21$mag are older than 13 Gyr and spend up to 10 Gyr of their overall evolutionarytime in the BC before they reach the RS migrating through the GV. Fainter ETGsare younger, of about 2 Gyr on average, and evolve for about 7-8 Gyr along theBC. The turn-off occurs at z ~ 0.3-0.4. Therefore these ETGs spend up to 3-5Gyr crossing the GV; UGC 06324, the faintest ETG in the sample, still is in theGV. The mechanism driving their evolution is gravitational, due to mergingand/or interaction. Our SPH simulations suggest that ETG members of thesegroups evolved toward the RS before and during the group collapse phase. Thisresult is consistent with the dynamical analysis of both groups showing thatthey are not yet virialized.

The ($NUV-r$) vs. $M_r$ as a tracer of early-type galaxies evolution in USGC U376 and LGG 225 groups