  The infall and merger scenario of massive clusters in the Milky Way's
potential well, as one of the Milky Way formation mechanisms, is reexamined to
understand how the stars of the merging clusters are redistributed during and
after the merger process using, for the first time, simulations with a high
resolution concentrated in the 300 pc around the Galactic center. We adopted
simulations developed in the framework of the "Modelling the Evolution of
Galactic Nuclei" (MEGaN) project. We compared the evolution of representative
clusters in the mass and concentration basis in the vicinity of a supermassive
black hole. We used the spatial distribution, density profile, and the $50\%$
Lagrange radius (half mass radius) as indicators along the complete simulation
to study the evolutionary shape in physical and velocity space and the final
fate of these representative clusters. We detect that the least massive
clusters are quickly (<10 Myr) destroyed. Instead, the most massive clusters
have a long evolution, showing variations in the morphology, especially after
each passage close to the supermassive black hole. The deformation of the
clusters depends on the concentration, with general deformations for the least
concentrated clusters and outer strains for the more concentrated ones. At the
end of the simulation, a dense concentration of stars belonging to the clusters
is formed. The particles that belong to the most massive and most concentrated
clusters are concentrated in the innermost regions, meaning that the most
massive and concentrated clusters contribute with a more significant fraction
of particles to the final concentration, which suggests that the population of
stars of the nuclear star cluster formed through this mechanism comes from
massive clusters rather than low-mass globular clusters.
