where M$_{S}$ , A$_{κ,λ,ρ}$ and a$_{S}$ are soft SUSY-breaking mass parameters of order M$_{SUSY}$ ∼ 1 TeV. The second term in Eq. (267) induces the µ -term when when the scalar component of S acquires a VEV, µ = λ 〈 S 〉 ≈ λ 2 κ | A$_{κ}$ − a$_{S}$ | , where the VEVs of H$_{u,d}$ are neglected compared to the VEV of X$_{1}$$_{,}$$_{2}$ . The third term in Eq. (267), 1 2 ρ$_{ij}$ S N$_{i}$N$_{j}$ , gives rise to an effective lepton-number-violating Majorana mass matrix, i.e. M$_{S}$ = ρ$_{ij}$ v$_{S}$ . Assuming that ρ$_{ij}$ is approximately SO(3) symmetric, viz. ρ$_{ij}$ ≈ ρ 1$_{3}$ , one obtains 3 nearly degenerate right-handed neutrinos ν$_{1}$$_{,}$$_{2}$$_{,}$$_{3}$$_{R}$ , with mass m$_{N}$ = ρ v$_{S}$ . If λ and ρ are comparable in magnitude, then the µ -parameter and the SO(3)-symmetric Majorana mass m$_{N}$ are tied together, i.e. m$_{N}$ ∼ µ , thus leading to a scenario where the singlet neutrinos ν$_{1}$$_{,}$$_{2}$$_{,}$$_{3}$$_{R}$ can naturally have TeV or electroweak-scale masses. The renormalizable superpotential Eq. (267) of the model may be uniquely determined by imposing the continuous R symmetry: S → e $^{iα}$S , L → e $^{iα}$L , Q → e $^{iα}$Q with W → e $^{iα}$W , whereas all other fields remain invariant under an R transformation. Notice that the R symmetry forbids the presence of higher-dimensional operators of the form X$_{1}$X$_{2}$N$_{i}$N$_{j}$/M$_{P}$ . The crucial observation is that the superpotential Eq. (267) is symmetric under the permutation of the waterfall fields, X$_{1}$ ↔ X$_{2}$ . This permutation symmetry persists, even after the spontaneous SUSY breaking of U (1)$_{ξ}$, since in the ground state, 〈 X$_{1}$ 〉 = 〈 X$_{2}$ 〉 = M . Hence, there is an exact discrete symmetry acting on the gauged waterfall sector, similar to the D -parity. In order to break this unwanted D -parity, a subdominant FI D -term is required. As a D -parity conservation, heavy particles with mass gM are stable and can be considered cosmologically bad, if they are overproduced after the end of inflation. Furthermore, in order to avoid the SUGRA- η problem, the K¨ ahler potential has to be chosen of the form K = S 2 + κ$_{s}$ | S | $^{4}$/ 4 M 2 $_{P}$, where the Hubble induced mass correction to S field turns out to read ± 3 κ$_{s}$H $^{2}$S2 [662, 663], and the tree level potential is similar to F -term inflation models, reading in the limit S ≫ M , where the last term corresponds to the SUGRA correction assuming a minimal K¨ ahler potential. The cosmological predictions of the model are typical of any F -term inflation with so many free parameters at disposal, it is always possible to get the desired spectral tilt and the power spectrum. V$_{infl}$ ≃ κ $^{2}$M4 [ 1 + 1 64 π $_{2}$(4 κ 2 + 8 λ 2 + 6 ρ $^{2}$) ln( | S | $^{2}$/M$^{2}$) ] + M 2 $_{S}$S $^{2}$− ( κa $^{2}$M$^{2}$S +h . c . )+ κ $^{2}$M4 | S | 4 2 M$_{P}$ . (269) 124