SLAC-PUB-15334, SU/ITP-12/42 Anomalous dimensions and non-gaussianity 3 1 0 2 n Daniel Green(cid:7),♠, Matthew Lewandowski(cid:7), Leonardo Senatore(cid:7),♥,♠,(cid:70), Ja Eva Silverstein(cid:7),♥,♠, and Matias Zaldarriaga♣ 1 1 (cid:7) Stanford Institute for Theoretical Physics, Stanford University, Stanford, CA 94306, USA ] h ♥ SLAC National Accelerator Laboratory, 2575 Sand Hill, Menlo Park, CA 94025 t - p ♠ Kavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94025, USA e h (cid:70) [ CERN, Theory Division, 1211 Geneva 23, Switzerland 1 ♣ School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540, USA v 0 3 6 2 . 1 Abstract 0 3 Weanalyzethesignaturesofinflationarymodelsthatarecoupledtostronglyinteractingfieldthe- 1 : ories,abasicclassofmultifieldmodelsalsomotivatedbytheirroleinprovidingdynamicallysmall v i scales. Near the squeezed limit of the bispectrum, we find a simple scaling behavior determined X r by operator dimensions, which are constrained by the appropriate unitarity bounds. Specifically, a we analyze two simple and calculable classes of examples: conformal field theories (CFTs), and large-N CFTs deformed by relevant time-dependent double-trace operators. Together these two classes of examples exhibit a wide range of scalings and shapes of the bispectrum, including nearly equilateral, orthogonal and local non-Gaussianity in different regimes. Along the way, we compare and contrast the shape and amplitude with previous results on weakly coupled fields coupled to inflation. This signature provides a precision test for strongly coupled sectors cou- pled to inflation via irrelevant operators suppressed by a high mass scale up to ∼ 103 times the inflationary Hubble scale. Contents 1 Introduction and summary 2 2 Conformally Coupled Examples 5 2.1 Setup . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5 2.2 Calculating in-in Correlators in Euclidean Signature . . . . . . . . . . . . . . . . . 7 2.3 Corrections to the Power Spectrum . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 2.4 Bispectrum from (cid:104)OO(cid:105) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9 2.4.1 The Squeezed Limit . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11 2.4.2 The Shape and Amplitude of the Bispectrum . . . . . . . . . . . . . . . . . 12 2.5 Bispectrum from (cid:104)OOO(cid:105). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 2.5.1 The Squeezed Limit . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 2.5.2 The Shape and Amplitude of the Bispectrum . . . . . . . . . . . . . . . . . 17 2.6 The Collapsed Limit of the Tri-Spectrum . . . . . . . . . . . . . . . . . . . . . . . 18 2.6.1 The (cid:104)OO(cid:105)-induced Tri-Spectrum . . . . . . . . . . . . . . . . . . . . . . . . 19 2.6.2 The (cid:104)OOOO(cid:105)-induced Tri-Spectrum . . . . . . . . . . . . . . . . . . . . . . 20 3 Time Dependent Examples 23 3.1 Modular example . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24 4 Discussion and Future Directions 29 A Radiative Corrections 30 A.1 Case 1: Bispectrum determined by (cid:104)OO(cid:105) . . . . . . . . . . . . . . . . . . . . . . . 30 A.2 Case 2: Bispectrum determined by (cid:104)OOO(cid:105) . . . . . . . . . . . . . . . . . . . . . . 31 A.2.1 Relevant deformation: ∆ ≤ 2 . . . . . . . . . . . . . . . . . . . . . . . . . . 31 A.2.2 Irrelevant Deformation : ∆ > 2 . . . . . . . . . . . . . . . . . . . . . . . . . 33 A.3 Case 3: Trispectrum determined by (cid:104)OO(cid:105) . . . . . . . . . . . . . . . . . . . . . . . 34 B Details of the Shape Calculation 34 1 1 Introduction and summary In inflationary cosmology, the quantum fluctuations of the inflaton, and possibly other fields, get imprinted on the power spectrum and higher point correlations accessible in the CMB and large- scale structure. This basic idea goes back to the origins of the subject, and has been explored in many illustrative examples. Recently there has been progress toward a more systematic un- derstanding of the observables and their implications, with input both from bottom up effective field theory and from top down UV complete mechanisms for inflation. In this paper, we mix in a basic class of strongly-coupled fields – field theories which are conformal at the Hubble scale and their time-dependent deformations – and compute their con- tribution to the perturbation spectrum and non-Gaussianity. We find characteristic scaling be- havior depending on the anomalous dimensions of operators, and compute in detail the shape and amplitude of the non-Gaussianity. The results depend on some basic properties of quantum field theory, such as unitarity bounds and crossing relations. Aside from theoretical interest, this analysis is motivated by several considerations. First, it is a canonical and calculable regime of field theory which belongs in a systematic analysis of multifield signatures and their significance, particularly given the observational handles on non-Gaussianity. Relatedly, as we will see, these strongly coupled sectors exhibit an interesting partial degeneracy with weakly interacting fields in their predictions for the simplest practical observables. Finally, from the top down, strongly coupled sectors play a useful role in model- building, producing naturally small scales in the effective action for the inflaton, and fields from this sector may participate in the perturbations. More generally, we can use forthcoming non- Gaussianitydata(whetheraconstraintordetection)toprovideaprecisiontestofadditionalfield theory sectors which couple to inflation via higher dimension operators. To put this in context, one basic question probed by observations is the number of fields which participate in generating the correlation functions of the curvature perturbations. This is adifferentquestionfromthequestionofhowmanyfieldsareinvolvedintheunderlyingmechanism producing the inflationary background. One can separate multi-field theories into two classes, depending on whether the additional fields themselves acquire scale invariant perturbations that affect the curvature or the isocurvature fluctuations. In the case we will be interested in here, the additional fields instead affect the density perturbations through their couplings to the inflaton. Thoughnotdirectlyobservable, theseadditionalfieldscannotusefullybeintegratedout, asdoing so would lead to a non-local Lagrangian. Progress toward a general treatment of both types of theories can be found in [1][2], where the effects of additional sectors are packaged in terms of their correlation functions. A useful general theorem known as the consistency condition establishes that a single-field theoryofperturbationscannotgeneratenon-Gaussianityinthe‘squeezed’configuration,withone mode much longer than the others [3]. Conversely, it has been long known that non-Gaussianity peaked in the squeezed configuration can arise in the presence of additional light fields [4]. For massless weakly interacting fields coupled to the inflaton, the three point function of scalar perturbations behaves as f ∆4 (cid:104)ζ ζ ζ (cid:105) −k−1−(cid:28)−k−2−(cid:39)−k→3 NL ζ (2π)3δ(3)(k +k +k ) (1.1) k1 k2 k3 k3k3 1 2 3 1 2 2 where ∆ ≈ 10−5 is the amplitude of the scalar perturbation. Moreover, interesting power-law ζ deviations from this shape of non-Gaussianity arise for fields of nonzero mass m [5] (cid:104)ζ ζ ζ (cid:105) = B(k ,k ,k ) (2π)3δ(3)(k +k +k ) (1.2) k1 k2 k3 1 2 3 √ 1 2 3 −k−1−(cid:28)−k−2−(cid:39)−k→3 fNL∆4ζ ×(cid:18)k1(cid:19)3/2− 9/4−m2/H2 (2π)3δ(3)(k +k +k ) (1.3) k3k3 k 1 2 3 1 2 2 This scenario, known as quasi single-field inflation, is a feature of weakly coupled theories with supersymmetry broken at the Hubble scale [6]. In the present work, we will analyze two simple cases where the additional fields affecting the density perturbations are strongly interacting, using conformal symmetry and related methods to control the calculations. For our first class of examples, we will study inflation coupled to a conformally coupled CFT, for which the conformal dimension ∆ of an operator O plays the role of the mass-dependent exponent in (1.3). For our second class of examples we will consider a simple time-dependent flow away from a large-N CFT, which gives unitary theories realizing a larger range of exponents, including local f . NL For our first class of examples, a conformally coupled CFT linearly mixes with inflaton per- turbations 1 , giving rise to a bispectrum of the form B(k ,k ,k ) −k−1−(cid:28)−k−2−(cid:39)−k→3 fNL∆4ζ ×(cid:18)k1(cid:19)∆ (∆ ≤ 2) (1.4) 1 2 3 k3k3 k 1 2 2 −k−1−(cid:28)−k−2−(cid:39)−k→3 fNL∆4ζ ×(cid:18)k1(cid:19)2 (∆ ≥ 2) . k3k3 k 1 2 2 For this case, the standard unitarity bound implies ∆ ≥ 1. As a result, the shape is peaked at equilateral/flattened triangles in momentum space, with the scaling behavior (1.4) as one approaches the squeezed limit determined by the dimension of the most relevant operator that couples in. Moreoever, we will find a range of exponents arising from dimensions 3/2 ≤ ∆ ≤ 2 which cannot be obtained in quasi-single field models, producing a scale-dependent bias which could distinguish them. For the range of exponents where the two are degenerate, it is intriguing that our intrinsically gapless CFT fields behave like massive weakly coupled fields with respect to the squeezed limit; the origin of this effect is the redshifting of conformally rescaled correlators of our conformally coupled operators. The conformal coupling to curvature which goes into this analysis is a special choice, and we expect a wider range of behaviors in the presence of more general curvature couplings. Indeed, our second class of examples will give rise to the same scaling2 as (1.4) while allowing for ∆ < 1. These examples make use of the fact that time-dependent couplings in quantum field theory can strongly affect infrared physics and shift unitarity bounds, as studied recently in [7]. This is important in the present context since time dependent couplings can arise very easily via couplings of the rolling inflaton field to other sectors such as a CFT. In the examples in [7], time dependent couplings can introduce flows between a unitary CFT containing an operator O 1Note that our CFT lives in the four-dimensional spacetime, and is not to be confused with conjectural lower- dimensional holographic duals for de Sitter. 2up to logarithmic factors. 3 of dimension ∆+ and an infrared theory with two-point correlators falling off like 1/distance2∆− times powers of the time-dependent coupling, where ∆ = 4−∆ . In particular a theory with − + a marginal scalar operator with ∆ ≈ 4 can flow in this way to a theory with ∆ (cid:28) 1, giving + − nearly local non-Gaussianity, not suppressed in the squeezed limit by any additional powers of k /k . 1 2 Finally, let us discuss the amplitude f of the bispectrum. As we will see, this can be NL substantial, and will give us sensitivity to higher dimension couplings of the inflationary sector to other fields. To give a rough illustration of this last point, consider, for example, a dimension ∆ = 2 operator O in a CFT, coupled to the inflaton φ via the dimension six operator 2 (cid:90) √ (∂φ)2O d4x −g 2 . (1.5) M2 ∗ Let us evaluate one factor of ∂φ on the backround rolling scalar field, which in slow-roll inflation given in terms of the inflationary Hubble scale H by φ˙ ∼ H2/∆ ∼ 105H2. This gives us a 0 ζ linear mixing (cid:82) ∆−1(H/M )2δφ˙O between the canonical perturbation δφ and O.3 The CFT ζ ∗ three-point function combined with three of these mixing interactions generates a contribution to the three-point function of the inflationary perturbations. This leads to an amplitude f NL behaving parametrically like (cid:18) H (cid:19)6 f ∼ C∆−4f(2) (1.6) NL ζ M ∗ where C is the amplitude of the CFT three-point function (2.1), and the function f(∆), plotted below in Fig. 6, gives a substantial numerical factor.4 Since current measurements are projected to be sensitive to f (cid:46) 10, they provide a precision test of this higher dimension coupling NL up to a value of M ∼ 103H. This high mass scale (relative to Hubble) is generally below the ∗ Planck scale (M ), but can exceed the GUT scale in simple examples such as chaotic inflation. pl In string-theoretic ultraviolet completions of inflation, higher dimension operators suppressed by a scale M (cid:28) M of order the Kaluza-Klein or string scale may be probed.5 That is, while an ∗ pl observation of non-Gaussianity may be explained by contributions from additional fields (weakly or strongly coupled), a null result would conversely provide a precision constraint on very high- energy physics. Of course sensitivity to high energy physics arises already in single field inflation (see e.g. [12, 13, 14, 15]). A feature of the present case is that observations will constrain hidden sectors of additional fields coupled to inflation via higher dimension operators such as (1.5). Similar constraints arise in other models involving a linear mixing with the inflaton (e.g. [5, 16]). Both of our main examples are just calculable examples of a wider point: additional fields active during inflation may include strongly coupled sectors with characteristic signatures. It 3Forthepurposesoffindingasimpleestimateofoursensitivitytohighdimensioncouplings,wewilltuneaway therelevantperturbationoftheCFTthatwegetfrom(1.5)ifweevaluatebothfactorsof∂φontherollinginflaton background. InthedetailedexamplestobediscussedinthemainbodyofthispaperandappendixA,wewillfind similar results without such tuning. 4Below we will describe our normalization conventions which go into this. 5InseveraloftheUVcompletionsofinflationexploredextensivelyinstringtheory,reviewedforexamplein[8], strongly coupled sectors play a useful role in producing dynamically small scales [9]. Operators suppressed by the Kaluza-Klein scale are ubiquitous there [10]. (See [11] for some more recent examples in which interacting field theory plays a role in the inflationary mechanism.) 4 will be interesting to analyze this more generally and systematically, and also to incorporate the particular couplings arising in complete models of inflation which involve couplings to strong dynamics to obtain their specific multifield signatures. 2 Conformally Coupled Examples In this section, we will consider strongly coupled theories which behave like a CFT near the inflationaryHubblescale. Inflatspacetime,CFTsareoneofthebeststudiedclassesofinteracting field theories. Due to the high degree of symmetry, much is known about the spectrum of operators and their correlations functions. Because de Sitter space is conformally flat, a CFT can be coupled to gravity such that correlation functions in de Sitter space preserve the flat space results up to an overall rescaling. This choice is related to the choice of curvature couplings involving operators in the CFT (or equivalently to the choice of improvement terms for the stress tensor that we couple to gravity). In this section, we will assume these couplings are chosen to preserve conformal invariance. 2.1 Setup WeareinterestedinthepossibilitythataCFTisweaklycoupledtotheinflatonanditsperturba- tion. As a result, the CFT will influence the correlation functions of the curvature perturbation we observe at late times. For this purpose, it is not necessary to specify the underlying dynamics leading to inflation; instead it is most convenient to work directly in terms of the perturbations π(t,(cid:126)x) as in the effective field theory treatment developed in [14]. Indeed, the effects we wil compute could accompany a wide variety of underlying inflationary mechanisms. Intheabsenceofinflation,aCFTisdescribedbyalistoflocal,primaryoperatorsO(j,˜j),∆i(x,t) i and their correlation functions, where (j,˜j) ∈ (Z, Z) is the spin and ∆ is the dimension of the 2 2 i i-th operator. For simplicity we will focus on a single scalar operator O(x,t) with dimension ∆. Inflatspace, thetwo-andthree-pointfunctionsofO(x,t)arefixeduptoaconstant. Specifically, the correlation functions in Euclidean signature take the form 1 (cid:104)O(x,t)O(0)(cid:105) = , (2.1) |x2+t2|∆ C (cid:104)O(x ,t )O(x ,t )O(x ,t )(cid:105) = , (2.2) 1 1 2 2 3 3 ∆ ∆ ∆ |x2 +t2 |2 |x2 +t2 |2 |x2 +t2 |2 12 12 23 23 31 31 wherex = x −x , t = t −t andC isaconstant. Thenormalizationofthetwo-pointfunction ij i j ij i j is a convention 6. The metric of de Sitter space is given by ds2 = a(τ)2(−dτ2+dx2) . (2.3) 6Inthelimit∆=1, theCFTbecomesfree. Inthiscase, theconventionforthetwo-pointfunctiondiffersfrom the one of a free scalar field a factor of 4π2. This explains why our dimensionless functions have sometimes large numerical values. 5 where a(τ) = −1/(Hτ). This metric is conformally flat in terms of the conformal time τ. Therefore, we get the CFT correlation functions in de Sitter space from the flat space result by replacing t → τ and a Weyl transformation of O(x,t) → a(τ)−∆O(x,τ). In particular, the two and three point functions are given by (in Euclidean time): a(iτ)−∆a(iτ(cid:48))−∆ (cid:104)O(τ,x)O(τ(cid:48),x(cid:48))(cid:105) = (2.4) [(τ −τ(cid:48))2+(x−x(cid:48))2]∆ C a(iτ )−∆a(iτ )−∆a(iτ )−∆ 1 2 3 (cid:104)O(x ,τ )O(x ,τ )O(x ,τ )(cid:105) = (2.5) 1 1 2 2 3 3 |x2 +τ2 |∆/2|x2 +τ2 |∆/2|x2 +τ2 |∆/2 12 12 23 23 31 31 In particular, these correlation functions redshift at late times much like those of a weakly inter- acting massive field. These strongly coupled correlators are different from those that arise in the weakly coupled case [5][6]; the position space two point function for massive fields is a nontrivial hypergeometric function, distinct from the simpler function (2.4) except for the special case of a conformally coupled free scalar. We will now couple the inflationary perturbation π to this CFT via the interaction Hamilto- nian H = 1µ2−∆M |H˙|1/2(2π˙ −∂ π∂µπ)O+ 1M2|H˙|µ˜−∆(−2π˙ +∂ π∂µπ)2O . (2.6) int 2 pl µ 4 pl µ Here and elsewhere, f˙ = −Hτ df is a derivative with respect to FRW time t = −log(−Hτ)/H. dτ The scalar π ∼ δt is not canonically normalized; it is related to the canonically normalized7 (cid:113) perturbation π via π = π / 2M2H˙. It is also related to the conventionally normalized scalar c c pl perturbation ζ via ζ = −Hπ (at linear order). We also note here that at freezeout, the corre- sponding field amplitudes which will enter into the calculations below are ζ ∼ ∆ ∼ 10−5 and ζ π ∼ H. In the whole paper we will neglect the mixing with gravity, as it will give subleading c corrections. In a slow-roll model like (1.5), the parameters µ and µ˜ may be related to φ˙ and some higher scale, M (e.g. µ = φ˙/M with M2 (cid:29) φ˙ when ∆ = 1). However, there may be many other ∗ ∗ ∗ UV completions that also give rise to (2.6) where these scales have different origins. For this reason, we will work directly with µ and µ˜ throughout, as they are the parameters relevant to the phenomenology. When ∆ < 2 the leading contribution from the first term is a relevant deformation and therefore is perturbative when µ (cid:28) H. On the other hand, the second term is irrelevant for all dimensions consistent with unitarity and is therefore perturbative the µ˜ (cid:29) H. A priori, the second term may or may not contribute significantly to the bispectrum. We will therefore consider the two cases separately in section 2.4 and 2.5. For the special case of ∆ = 2, we should replace (µ/H)2−∆ with a dimensionless coupling λ: λ = lim (µ/H)2−∆, with log(µ/H) → ∆→2 (λ−1)/(∆−2). This replacement should be unambiguous so we will not do it explicitly. In Appendix A, we analyze the radiative stability of this setup. One result of that analysis is that under appropriate conditions the term ∼ (cid:82) m4−∆O generated by π loops satisfies m (cid:28) H, meaning that even for relevant operators (∆ < 4) we do not generate a flow away from the CFT 7Here we are assuming unit speed of sound, c ∼1. For general sound speed, the canonically normalized field s (cid:113) is given by π=c π / 2M2H˙. s c pl 6 over the scales of interest. This analysis is self-contained up to a scale Λ which can be (cid:29) H, leading to precision tests of higher dimension operators as anticipated in the introduction. 2.2 Calculating in-in Correlators in Euclidean Signature Throughout the paper, we will be interested in calculating in-in correlations functions of ζ evaluated at equal times. These can be computed perturbatively, using the interaction picture fields, stating from [17], (cid:90) τ0 (cid:16) (cid:17) (cid:90) τ0 (cid:104)T¯exp[i H (τ)a(τ)dτ] ζ (k ,τ )..ζ (k ,τ ) T exp[−i H (τ)a(τ)dτ](cid:105) , int int 1 0 int n 0 int −∞(1+i(cid:15)) −∞(1−i(cid:15)) (2.7) where we have assumed the Bunch-Davies vacuum and H (τ) = (cid:82) d3xa3(τ)H (τ,x). In order int int to simplify these calculations, we will follow the strategy suggested in [18]. The basic idea is that, after rotating the conformal time integrals via τ → ±iτ +τ , the in-in correlation becomes a E 0 (Euclidean) anti-time-ordered correlation function. Figure 1: The analytic continuation of the contour in conformal time (τ) from Lorentzian signature (blue) to Euclideansignature(red). Wecalculatethecorrelationfunctionsforoperatorsatτ0<0. Ourexpressionsinvolve branchcutsonlywhenReτ >0,whichensuresthiscontinuationiswelldefined. Starting from the i(cid:15) prescription in (2.7), which projects onto the interacting vacuum, the time and anti-time ordered exponentials should be rotated to opposite values of the Euclidean time. After doing this, we obtain (cid:90) τ0 (cid:16) (cid:17) (cid:90) τ0 (cid:104)T¯exp[i H (τ)a(τ)dτ] ζ (k ,τ )..ζ (k ,τ ) T exp[−i H (τ)a(τ)dτ](cid:105). (2.8) int int 1 0 int n 0 int −i∞+τ0 i∞+τ0 7 This we recognize as simply the anti-time ordered correlation function in Euclidean time (cid:16) (cid:90) i∞+τ0 (cid:17) (cid:104)T¯ ζ (k ,τ )..ζ (k ,τ )exp[i H (τ)a(τ)dτ] (cid:105) (2.9) int 1 0 int n 0 int −i∞+τ0 (cid:16) (cid:90) ∞ (cid:17) = (cid:104)T¯ ζ (k ,τ )..ζ (k ,τ )exp[− H (iτ +τ )a(iτ +τ )dτ ] (cid:105) . (2.10) int 1 0 int n 0 int E 0 E 0 E −∞ Provided we use the anti-time ordered, Euclidean Green’s function which we will compute mo- mentarily, the operator ordering is automatic. This analytic continuation is illustrated in figure 1. The anti-time-ordered Green’s functions for any two operators can be written as (cid:104)T¯O (τ)O (τ(cid:48))(cid:105) ≡ θ(τ(cid:48) −τ )(cid:104)O (τ)O (τ(cid:48))(cid:105)+θ(τ −τ(cid:48) )(cid:104)O (τ(cid:48))O (τ)(cid:105) , (2.11) 1 2 E E 1 2 E E 2 1 where θ(x) is the Heaviside step function. Following the usual quantization of a scalar in de Sitter space, we write the operator πˆ = π (τ)aˆ† +π∗(τ)aˆ with [aˆ ,aˆ† ] = (2π)3δ(k+k(cid:48)) and k k k k k k k(cid:48) H (1−ikτ) H (1+ikτ) π (τ) = eikτ ; π∗(τ) = e−ikτ . (2.12) k 2M |H˙|1/2 k3/2 k 2M |H˙|1/2 k3/2 pl pl (As usual, we conjugate π to obtain π∗ in our original Lorentzian signature calculation, before deforming our contour to lie along τ .) Notice that external factors of π (τ ) only have nonzero E k 0 contractions with factors of π˙ in H , so that we will only need c int (cid:16) (cid:17) H3 τ (cid:104)T¯ π˙ (iτ +τ ,k )π (τ ,k ) (cid:105) = − (1+ik τ E )(−iτ −τ )2e−k1|τE|(2π)3δ(k +k ). (2.13) c E 0 1 c 0 2 1 0 E 0 1 2 2k |τ | 1 E The appearance of the absolute values in the above expression does not obstruct the analytic continuationweperformedinwriting(2.8);theonlynon-analyticbehaviorappearsatthelocation oftheoperatorinsertions,τ = τ ,whichisfixedinourcontinuation. Alternatively,onecanchoose 0 the domains of integration in (2.7) to be manifestly time-ordered, which ensures the integrands are analytic in τ. As we discussed in the previous section, the CFT correlation functions in Euclidean signature may be be taken to be anti-time ordered. Therefore, when evaluating correlation functions we can use equations (2.4) and (2.5) with τ = iτ +τ (we will drop the in remainder of this i i,E 0 E section). Since we are interested in behavior the correlation functions at late times, we will take τ → 0 at the end of all our calculations. 0 2.3 Corrections to the Power Spectrum WiththecouplingHint ⊃ √12µ2−∆π˙cO,weexpectacorrectiontothepowerspectrumPζ ∼ ∆2ζ/k3 at order (µ)4−2∆. The action does not depend explicitly on time and therefore we expect this H correction to be scale invariant on general grounds. In this subsection, we will confirm this intuition with an explicit calculation. The correction to the power spectrum arises from (cid:90) δP = M2|H˙|µ4−2∆(cid:104)ζ (τ )ζ (τ ) dτ dτ a(τ +iτ )4a(τ +iτ )4 (2.14) ζ pl k 0 −k 0 1 2 0 1 0 2 × π˙ (τ +iτ )π˙ (τ +iτ )(cid:105) (cid:104)O (τ +iτ )O (τ +iτ )(cid:105)(cid:48) , k 0 1 −k 0 2 −k 0 1 −k 0 2 8 where the prime on (cid:104)OO(cid:105)(cid:48) indicates that we drop the (2π)3 times a delta function in momentum. We will use the identity 1 (2π)2Γ(2−∆) (cid:90) d4k = eik·x(k2)∆−2 , (2.15) (x2)∆ 4∆−1 Γ(∆) (2π)4 where x is a 4-vector. The two-point function of O can be written in momentum space as (cid:104)O (τ +iτ )O (τ +iτ )(cid:105)(cid:48) = (2.16) k 0 1 −k 0 2 (2π)2Γ(2−∆) (cid:90) dω a(τ +iτ )−∆a(τ +iτ )−∆ eiωτ12(k2+ω2)∆−2 . 4∆−1 Γ(∆) 0 1 0 2 2π Plugging back in (2.14) the two integrals in τ and τ can be done analytically, and we are left 1 2 withtheintegralinω tobedonenumerically. Thecorrectiontothepowerspectrumisthengiven by (cid:16)µ(cid:17)4−2∆ δP ≡ P (k) t(∆) (2.17) ζ ζ H where π241−∆Γ(2−∆) (cid:90) 1 t(∆) = − e−i(2τ˜0+π∆) dω˜ × (2.18) Γ(∆) (ω˜2+1)2+∆ (cid:104) (τ˜ +i)(ω˜ −i)ei(2τ˜0+π∆)(1−iω˜)∆Γ(∆−1,−τ˜ (ω˜ −i)) 0 0 +(τ˜ −i)(ω˜ +i)(1+iω˜)∆Γ(∆−1,−τ˜ (ω˜ +i))(cid:3) × 0 0 (cid:2)(τ˜ −i)(ω˜ −i)(1−iω˜)∆Γ(∆−1,τ˜ (ω˜ −i)) 0 0 (cid:105) +(τ˜ +i)(ω˜ +i)ei(2τ˜0+π∆)(1+iω˜)∆Γ(∆−1,τ˜ (ω˜ +i)) , 0 0 where Γ[s,x] ≡ (cid:82)∞ts−1e−tdt is the upper incomplete gamma function, and where we take τ˜ = x 0 τ /k → 0 at the end of the calculation. In the limit τ˜ → 0, t(∆) is independent of k and 0 0 therefore the power spectrum remains scale invariant. The function t(∆) is plotted in figure 2. Notice that its numerical value is quite large, though the correction to the power spectrum is safely much smaller than one for a large range of values for µ. The large value is partly related to our conventions in equation 2.1, which differ from free field conventions by a factor of 4π2 (cid:39) 39.5. Further, notice the divergence as ∆ → 2. This is due to the necessity of a divergent counter-term for the two point function for ∆ ≥ 2. In the language of the EFT of Inflation, the unitary gauge operatorthatprovidesthecounter-termis(δg00)2 [19]. Uponre-insertionofπ,thistermscontains indeed the quadratic term π˙2. We see that a speed of sound different from unity is generated. We discuss about radiative corrections and renormalization in larger detail in Appendix A. We conclude that, upon renormalization, the contribution is small even for ∆ > 2. 2.4 Bispectrum from (cid:104)OO(cid:105) Let us begin to explore signatures in the bispectrum. The simplest case to compute is when the bispectrum in π (and so in ζ) is induce by the power spectrum (two point function) of O’s. This 9