this leads to the scalar potential [720] V = M 4 F ln ( φ 2 M 2 S ) + A cos( nθ + θ$_{A}$ ) λ$_{n}$φ n nM n − 3 GUT + λ 2 n φ 2( n − 1) M 2( n − 3) GUT , (338) where M$_{F}$ ∼ ( m$_{SUSY}$ × M$_{S}$ ) 1 / 2 and m$_{SUSY}$ ∼ 1 TeV is the soft SUSY breaking mass at the weak scale. For φ > M 2 $_{F}$/m$_{3}$$_{/}$$_{2}$ , usually the gravity mediated contribution, m 2 3 / $_{2}$φ$^{2}$, dominates the potential where m$_{3}$$_{/}$$_{2}$ is the gravitino mass. Here we will concentrate on the VEVs such that M$_{s}$ ≪ φ ≤ M 2 $_{F}$/m$_{3}$$_{/}$$_{2}$ . A successful inflation can be obtained near the point of inflection; φ$_{0}$ ≈ ( M n − 3 $_{GUT}$M 2 F λ$_{n}$ √ n ( n − 1)( n − 2) ) 1 / ( n − 1) , (339) A ≈ 4( n − 1) $^{2}$λ$_{n}$ nM n − 3 GUT φ n − 2 0 . (340) In the vicinity of the inlection point, the total energy density is given by V ( φ$_{0}$ ) ≈ M 4 F [ ln ( φ 2 0 M 2 S ) − 3 n − 2 n ( n 1) ] , (341) There are couple of interesting points, first of all note that the scale of inflation is extremely low, the Hubble scale during inflation is given by: H$_{inf}$ ∼ M 2 $_{F}$/M$_{P}$ ∼ 10 − 3 − 10 − 1 eV for M$_{F}$ ∼ 1 − 10 TeV. The relevant number of e-foldings is N$_{Q}$ ∼ 40 [720]. For M$_{F}$ ∼ 10 TeV, and φ$_{0}$ ∼ 10 11 GeV it is possible to match the CMB temperature anisotropy and the required tilt in the spectrum [720]. The validity of Eq. (338) for such a large VEV requires that M 2 F > (10 11 GeV) × m$_{3}$$_{/}$$_{2}$ . For M$_{F}$ ∼ 10 TeV this yields a bound on the gravitino mass, m$_{3}$$_{/}$$_{2}$ < 1 − 10 MeV, which is compatible with the warm dark matter constraints. B. Quantum stability 1. Radiative correction Since the MSSM inflaton candidates are represented by gauge invariant combinations of squarks and sleptons, the inflaton parameters receive corrections from gauge interactions which can be computed in a straightforward way. Quantum corrections result in a logarith- mic running of the soft SUSY breaking parameters m$_{φ}$ and A . The effective potential at 154