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Tensor to scalar ratio and large scale power suppression from pre-slow roll initial conditions

We study corrections to the power spectra of curvature and tensor perturbations and the tensor-to-scalar ratio in single field slow roll inflation due to initial conditions imprinted by a fast-roll stage prior to slow roll. For a wide range of initial inflaton kinetic energy, this stage lasts only a few e-folds and merges smoothly with slow-roll leading to non-Bunch-Davies initial conditions for modes that exit the Hubble radius during slow roll. We describe a program that yields the dynamics in the fast-roll stage while matching to the slow roll stage independent of the inflationary potentials. Corrections to the power spectra are encoded in a transfer function $\mathcal{T}_α(k)$. We obtain $\mathcal{T}_α(k)$ to leading order in a Born approximation valid for modes of observational relevance today. A fit yields $\mathcal{T}_α(k) =1+ A_αk^{-p}\cos[2πωk/H_{sr}+φ_α]$, with $1.5 \lesssim p \lesssim 2$, $ω\simeq 1$ and $H_{sr}$ the Hubble scale during slow roll inflation, where curvature and tensor perturbations feature the same $p,ω$ for a wide range of initial conditions. These corrections lead to both a suppression of the quadrupole and oscillatory features in both $P_R(k)$ and $r(k_0)$ with a period of the order of the Hubble scale during slow roll inflation. The results are independent of the specific inflationary potentials, depending solely on the ratio of kinetic to potential energy $κ$ and the slow roll parameters to leading order. For a wide range of $κ$ and the values of $ε_V;η_V$ corresponding to the upper bounds from Planck, we find that the low quadrupole is consistent with the results from Planck, and the oscillations in $r(k_0)$ could be observable if the modes corresponding to the quadrupole and the pivot scale crossed the Hubble radius a few e-folds after the onset of slow roll.