112 We now turn to the case α = 1 . We have given results only for the case Γ$_{ϕ}$ ≪ H$_{TI}$ . The reason for this is that this case yielded more liberal constraints than the case Γ$_{ϕ}$ ≳ H$_{TI}$ . For reasonable values of $^{H}$∗ and Γ$_{ϕ}$ , a value of g =0 . 4 yields a sharp prediction to within an order of magnitude for all but one of the quantities in the model, regardless of the $^{φ}$∗ case. The quantity m$_{ψ}$ can span many orders of magnitude when looking within the range m$_{0}$ ∼ 10 $^{2}$– 10 3 GeV and we report only an upper bound of m$_{ψ}$ ∼ 10 − $^{4}$– 10 − 2 GeV. Regarding the tensor fraction, we obtain a prediction of r ∼ 10 − 13 for a value of $^{H}$∗ ∼ 10 8 GeV. We also report values for the non-Gaussianity parameters f$_{NL}$ and g$_{NL}$ for local-type non-Gaussianity, i.e. for when the momenta triangle is in the squeezed configuration. We predict values of f$_{NL}$ ∼ 10 − 1 and g$_{NL}$ ∼ 10 − $^{2}$, for a value of m$_{0}$ ∼ 10 3 GeV, which are within current observational bounds. In order to obtain predictions from our model for the scalar spectral index and its running, we needed to choose an inflation model for the period of pri- mordial inflation. We chose to use a simple slow-roll Chaotic Inflation model, with the potential given by Eq. (4.174). We obtain values of n$_{s}$ ≈ 0 . 9645 and n ′ s ≈ − 0 . 001259 , for values of m$_{0}$ ∼ 10 3 GeV, N$_{TI}$ ≈ 24 and $^{N}$∗ ≈ 28 and independent of the $^{φ}$∗ Case and the value of m$_{ψ}$ within its allowed range. These values for n$_{s}$ and n ′ s are within current observational bounds. As already mentioned, the analysis that we have performed on our model has been limited to a relatively small region of the vast parameter space. Therefore, it is possible that there exist other allowed regions, for different values of some or all of the free parameters in the model. This is a potential area for future research. In addition, as our analysis has been purely analyti-