Small field inflationary models: a revival

We numerically study scale dependence of the cosmic microwave background (CMB) power spectrum in a class of small, single-field models of inflation which lead to a high value of the tensor to scalar ratio. The inflaton potentials that we consider are degree 5 and 6 polynomials, for which we calculate the power spectrum numerically and extract the cosmological parameters: the scalar index n_s , the running of the scalar index n_run , the running of running n_run,run , and the tensor to scalar ratio r . We show that we are able to produce single small field models which yield a tensor to scalar ratio of up to r=0.01 , which additionally conform to most recent known values of the CMB observables. 

Gravitational Wave generating potentials conforming to known CMB observables