Abstract　 　　 

　The system conformed by the Milky-Way and its satellite galaxies is the most studied and most commonly employed system to test and/or interpret different cosmological scenarios. Within the current paradigm of structure formation, LCDM scenario, the hierarchical formation of virialized halos is through the accretion of both diffuse mass and of smaller halos. At the same time, galaxies formed within these dark matter halos where multiple feedback mechanisms are thought to be responsible for setting up their observational properties. Thus, one expects that the observed population of galaxies should be the result of the halo assembly history. If this is so, Does the LCDM scenario reproduce the observed abundances of satellite galaxies around Milky-Way sized galaxies?. Is the LCDM scenario capable to predict the observed likelihood of Milky-Way like systems? Are the internal dynamics of subhalos consistent with observations based on the Milky-Way satellites? In this talk I will present several occupational distributions for Milky-Way sized galaxies inferred based on the LCDM scenario. While our analysis suggest that the abundance of massive subhalo agrees with the abundance of massive satellites in Milky-Way sized hosts (i.e. ,no missing massive satellite problem), we confirm that the maximum circular velocity of subhalos is systematically large than what is suggest by observational studies based on the Milky-Way satellites.