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From our potential, Eq. (4.2), we have 

Substituting the VEV of φ , Eq. (4.7), into here gives 

for all reasonable values of n . Therefore, we require 

## 4.4.3.4 Light ψ 

<img src='content_image/304102.jpg'>

<img src='content_image/304101.jpg'>

<img src='content_image/304100.jpg'>

In order that ψ acquires classical perturbations during primordial inflation, we require the effective mass of ψ to be light during this time, i.e. 

where we are using notation such that | m$_{ψ,}$$_{eff}$ | ≡ √ ∣ m 2 ψ, eff ∣ . We have 

Therefore we require 

<img src='content_image/304097.jpg'>

<img src='content_image/304099.jpg'>

<img src='content_image/304098.jpg'>

