Globular Clusters in the Galactic Center Region: expected behavior in the infalling and merger scenario

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