G$_{0}$ and Λ$_{0}$ are the non–improved coupling constants. Indeed, at the fixed point regime , i.e. k ≫ m$_{pl}$ (where m$_{pl}$ = G − 1 2 0 is the Planck mass), the numerical analysis suggests where g UV ∗ = 0 . 27 and λ UV ∗ = 0 . 36 are the non–Gaussian fix point values of dimensionless couplings g ( k ) ≡ k $^{2}$G ( k ) and λ ( k ) ≡ Λ( k ) k 2 , respectively. In the following, we are dealing with the end of the inflation epoch with k ≲ m$_{pl}$ , and thus it is logical to use the perturbative regime. Hence we use the (3) and (4) as the running couplings for this period. As it is the case for any quantum field theory, running couplings are scaled with momentum k . On the other hand, in effective field theory, Γ$_{k}$ uses this scaling to specify the cutoff point where the fluctuations with momenta smaller than k are ignored. In the space–time picture this cutoff momentum should be related to the inverse of some physical length. Generally speaking, using isotropy and homogeneity of FRW metric, a suitable function k ( t, a ( t ) , ˙ a ( t ) , ... ) seems to be the best choice for scaling parameter. Noting that in the standard cosmology, when the Universe is aged t , fluctuations of frequency smaller than 1 /t are ignorable, and also taking into account the dimensional considerations, one observes that the cutoff identification is a suitable approximation. Here ξ is a positive constant of order unity. (This may also be justified for the fixed point regime, where Λ( k ) ∝ k $^{2}$., and since we know that Λ ∝ H $^{2}$( t ). See [14].) One may also uses the conformal time ∫ dt/a ( t ) instead of t , but the difference is ignorable because of ignorance of frequencies less than 1 /t . As a result, the above cutoff identification is usually used for improvement of the cosmological models in the literature. For more details about cutoff identification, the reader is referred to [11] and [15]. k = ξ t (5) 5 G ( k ) = g UV ∗ k 2 , Λ( k ) = λ UV ∗ k 2