An appealing explanation for the Planck data is provided by inflationary models with a singular non-canonical kinetic term: a Laurent expansion of the kinetic function translates into a potential with a nearly shift-symmetric plateau in canonical fields. The shift symmetry can be broken at large field values by including higher-order poles, which need to be hierarchically suppressed in order not to spoil the inflationary plateau. The herefrom resulting corrections to the inflationary dynamics and predictions are shown to be universal at lowest order and possibly to induce power loss at large angular scales. At lowest order there are no corrections from a pole of just one order higher and we argue that this phenomenon is related to the well-known extended no-scale structure arising in string theory scenarios. Finally, we outline which other corrections may arise from string loop effects.

Working in the Large Volume Scenario (LVS) of IIB Calabi-Yau flux compactifications, we construct inflationary models from recently computed higher derivative (α ) 3 -corrections. Inflation is driven by a Kähler modulus whose potential arises from the aforementioned corrections, while we use the inclusion of string loop effects just to ensure the existence of a graceful exit when necessary. The effective inflaton potential takes a Starobinsky-type form V = V 0 (1 − e −νφ ) 2 , where we obtain one set-up with ν = −1/ √ 3 and one with ν = 2/ √ 3 corresponding to inflation occurring for increasing or decreasing φ respectively. The inflationary observables are thus in perfect agreement with PLANCK, while the two scenarios remain observationally distinguishable via slightly varying predictions for the tensor-to-scalar ratio r. Both set-ups yield r (2 . . . 7) × 10 −3 . They hence realise inflation with moderately large fields (∆φ ∼ 6 M P l ) without saturating the Lyth bound. Control over higher corrections relies in part on tuning underlying microscopic parameters, and in part on intrinsic suppressions. The intrinsic part of control arises as a leftover from an approximate effective shift symmetry at parametrically large volume.ArXiv ePrint: 1509.00024 arXiv:1509.00024v2 [hep-th]

Motivated by UV realisations of Starobinsky-like inflation models, we study generic exponential plateau-like potentials to understand whether an exact f (R)formulation may still be obtained when the asymptotic shift-symmetry of the potential is broken for larger field values. Potentials which break the shift symmetry with rising exponentials at large field values only allow for corresponding f (R)descriptions with a leading order term R n with 1 < n < 2, regardless of whether the duality is exact or approximate. The R 2 -term survives as part of a series expansion of the function f (R) and thus cannot maintain a plateau for all field values.We further find a lean and instructive way to obtain a function f (R) describing m 2 φ 2 -inflation which breaks the shift symmetry with a monomial, and corresponds to effectively logarithmic corrections to an R + R 2 model. These examples emphasise that higher order terms in f (R)-theory may not be neglected if they are present at all. Additionally, we relate the function f (R) corresponding to chaotic inflation to a more general Jordan frame set-up. In addition, we consider f (R)-duals of twogiven UV examples, both from supergravity and string theory. Finally, we outline the CMB phenomenology of these models which show effects of power suppression at low-ℓ.

Inflationary attractors predict the spectral index and tensor-to-scalar ratio to take specific values that are consistent with Planck. An example is the universal attractor for models with a generalized nonminimal coupling, leading to Starobinsky inflation. In this paper we demonstrate that it also predicts a specific relation between the amplitude of the power spectrum and the number of e-folds. The length and height of the inflationary plateau are related via the nonminimal coupling: in a wide variety of examples, the observed power normalization leads to at least 55 flat e-foldings. Prior to this phase, the inflationary predictions vary and can account for the observational indications of power loss at large angular scales.

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