density dependence of the meson-nucleon coupling operators [@tw; @ring1]. Moreover, density dependent hadronic models can also be a useful tool in obtaining EoS for neutron stars even if hyperons are to be considered [@ddpeos], which is not the case if NL3 or TM1 are used. Both, NL3 and TM1, can only be used if the EoS is restricted to accommodate neutrons, protons and the leptons necessary to enforce $\beta$-stability. Once hyperons are included, the nucleons acquire a negative effective mass above $\sim 3-4 \rho_0$ densities [@compact; @alex], where $\rho_0$ is the nuclear saturation density.

The second model, that we refer to as NL$\omega\rho$ model, includes non-linear $\sigma-\rho$ and $\omega-\rho$ couplings [@hp01; @hp2001; @bunta; @bunta2] which allow to change the density dependence of the symmetry energy of the most common parametrizations of the NLWM that show essentially a linear behavior of the symmetry energy with density. However, the symmetry energy determines the behavior of isospin asymmetric matter and therefore is intrinsically related to the characteristics of the EoS that can describe neutron stars. Within this model the authors of [@hp01] have shown that the neutron skin thickness of $^{208}Pb$ was sensitive to the isovector channel of the nuclear interaction and there 