Kaluza–Klein reductions and AdS/Ricci-flat correspondence

The AdS/Ricci-flat (AdS/RF) correspondence is a map between families of asymptotically locally AdS solutions on a torus and families of asymptotically flat spacetimes on a sphere. The aim of this work is to perturbatively extend this map to general AdS and asymptotically flat solutions. A prime application for such map would be the development of holography for Minkowski spacetime. In this paper we perform a Kaluza–Klein (KK) reduction of AdS on a torus and of Minkowski on a sphere, keeping all massive KK modes. Such computation is interesting on its own, as there are relatively few examples of such explicit KK reductions in the literature. We perform both KK reductions in parallel to illustrate their similarity. In particular, we show how to construct gauge invariant variables, find the field equations they satisfy, and construct a corresponding effective action. We further diagonalize all equations and find their general solution in closed form. Surprisingly, in the limit of large dimension of the compact manifolds (torus and sphere), the AdS/RF correspondence maps individual KK modes from one side to the other. In a sequel of this paper we will discuss how the AdS/RF maps acts on general linear perturbations.


Introduction
The advent of the holographic principle [1,2], and its precise realization in the form of the AdS/CFT correspondence [3,4], has provided us with deep insights into the nature of spacetime and gravitational forces. This was enabled by special properties of anti-de Sitter (AdS) gravity, that grant better control on the asymptotic structure of solution to the field equations [5], and allows to develop very effective tools [6]. Notably, we now have a well-developed holographic dictionary that allows us to translate gravitational questions to quantum field theory (QFT) ones and vice versa, a good understanding of AdS black holes, a precise fluid/gravity correspondence, and (in principle) a full, non-pertubative formulation of quantum gravity on AdS in terms of the dual CFT. Gravitational techniques are now commonly applied to tackle field theoretic questions, such as the quark-gluon plasma, strongly interacting condensed matter systems, and quantum information problems (see e.g. [7][8][9] and references therein). Following the inverse path, the dual QFT is currently our best window to investigate fundamental questions such as the emergence of spacetime, causality, and the resolution of singularities.
Such questions are out of our reach when leaving the safe harbour of AdS spacetimes for asymptotically (locally) flat (ALF) spacetimes. The holographic principle is still expected to play a key role, but its formulation for such spacetimes still eludes us despite the existence of general arguments for holography and various attempts to implement it (see [10][11][12][13][14][15][16][17][18][19][20] for a sample of works). On the other hand, and in a somewhat complementary way, other aspects of ALF physics have been developed in great extent over the years. For example, we have much better control of quantum field theory on curved spacetimes when the background spacetime is asymptotically flat. The reason is that general relativistic effects become negligible in the asymptotic regions, and the QFT Hilbert space for initial and final states can be constructed in a familiar way. Hence, one can define an S-matrix relating in and out states. Such a construction is not readily available for asymptotically AdS spacetimes (see e.g. [21]). Moreover, asymptotically flat spacetimes enjoy a large symmetry group, the Bondi, van der Burg, Metzner, Sachs (BMS) group [22,23]. This asymptotic symmetry has recently resurfaced [24] (see [25] for a review and further references) in relation to gravitational scattering and Weinberg's soft theorems [26], and as the carrier of the soft hair that has been conjectured to solve the black hole information problem in [27,28]. The perturbative superstring theory itself can be defined and quantized much more easily on Minkowski spacetime than on an AdS background. Last but not least, asymptotically flat spacetimes benefit from various integrability properties and solution generating techniques (see e.g. [29] for a review), which are not available in the presence of a non-vanishing cosmological constant.
It is therefore clear that if one could construct a bridge between asymptotically flat and asymptotically AdS spacetimes, there would be great gains for both sides, since concepts and tools could be transferred from one to another by crossing over it. The foundation for such a bridge was sketched in [30], in the form of the Anti-de Sitter/Ricci-flat correspondence.
The Anti-de Sitter/Ricci-flat (AdS/RF) correspondence is, at its heart, a simple geometrical map between families of Einstein manifolds. It can be used to map families of solutions of AdS gravity to families of solution of vacuum Einstein gravity, and has therefore the potential to enlighten us upon the formulation of holography on Ricci-flat manifolds by mapping to them the well-known holographic tools developed in the context of AdS/CFT. This line of thought was pursued with success in [31], where holographic boundary conditions and 2-point functions in Minkowski spacetime were obtained from AdS compactified on a torus, and the hydrodynamic regime of asymptotically flat black p-branes and the Rindler fluid [32][33][34][35] were linked to the conformal fluid dynamics described by the AdS fluid/gravity metrics [36].
Mathematically, the AdS/RF map is defined by the following recipe. The starting ingredient is a family of (d + 1)dimensional spacetimes that solves Einstein's equations with a negative cosmological constant = −d(d − 1)/2 2 (1.1) for any value of d, and consists of a flat (d − p − 1)dimensional torus warped over a ( p + 2)-dimensional base space. We can always choose coordinates y a (with a = 0, . . . , p + 1) on the base space, and coordinates χ i (with i = 1, . . . , d − p − 1) on the torus, such that its line element takes the form We can extract from this expression the ( p + 2)-dimensional metricĝ ab (y; d) and the scalar fieldφ(y; d), where we explicitly indicate that these coefficients may dependent on d. The next step is to define a new ( p + 2)-dimensional metricg ab (y; n) and a new scalar fieldφ(y; n), both depending on a new parameter n, as g(y; n) =ĝ(y; −n),φ(y; n) =φ(y; −n).
Finally, we construct a (n + p + 3)-dimensional metric by plugging the fieldsg ab (y; n) andφ(y; n) in the Ansatz ds 2 0 = e 2φ(y;n) n+ p+1 g ab (y; n) dy a dy b + 2 d 2 n+1 , (1.4) where d 2 n+1 is the unit metric of the round (n + 1)-sphere S n+1 . Then the metric associated to the line element (1.4) is Ricci-flat (RF), i.e. it solves Einstein's equations in vacuum. The map works in the other direction as well: starting from a family of (n + p + 3)-dimensional Ricci-flat manifolds that have a round sphere S n+1 warped over a ( p+2)-dimensional base, one casts their metrics in the form (1.4), reads off the metricg ab (y; n) and the scalar fieldφ(y; n), performs the substitution n → −d and replaces the outcome in the AdS Ansatz (1.2). Then, the resulting family of metrics solves Einstein's equations with the cosmological constant (1.1) for all values of d. This is illustrated by the diagram in Fig. 1. The reason why the map works is that the (consistent) diagonal dimensional reduction of an asymptotically AdS spacetime on a torus and that of a Ricci-flat spacetime on sphere down to p + 2 dimensions yields the same lower dimensional equations of motion, provided one matches the cosmological radius of AdS to the radius of the sphere and analytically continues d to −n. 1 The main message is that this map creates a first connection between AdS and RF manifolds, and we intend with our analysis to see up to what extend this connection can be exploited to bridge AdS physics to asymptotically flat spacetimes and back.
A major limitation of this approach stems from the AdS/RF map requirement that the AdS geometry has a flat torus, and correspondingly the Ricci-flat manifold contains a round sphere. This restricts the physical processes to which it can be applied. For example, while modes propagating on the extended directions of AdS black branes can be mapped to transverse modes of the corresponding Schwarzschild black branes, 2 the correspondence does not capture modes that deform the internal torus or sphere. This is a hurdle when studying for instance the Schwarzschild black hole: by Birkhoff's theorem we are freezing all the dynamics, and not much is left to be mapped! To understand holographically such modes by using similar methods, one has to extend the correspondence to allow for at least some extra modes living on these compact manifolds to be mapped into each other. A number of generalizations and extensions of the correspondence were studied in [39][40][41].
The task we undertake in this article is to find out whether such an extension of the original formulation of the AdS/RF correspondence is possible. To simplify the analysis, we will switch to a perturbative approach and restrict it to linear perturbations of the simplest occurrence of the map: that relating Minkowski spacetime and the Poincaré patch of AdS spacetime. It will be easier to crack the map for modes deforming the compact manifold in such a simplified setting. Moreover, the study of these linear perturbations is the first, necessary step towards translating the AdS/CFT dictionary to AF spacetimes, since these fluctuations of the metric determine the correlation functions of the dual CFT operators [42].
To be more precise, recall that the AdS/RF correspondence maps Ad S d+1 on the torus T d− p−1 (1.5) to n + p + 3 Minkowski spacetime, 1 Such analytic continuation in d was first introduced in [37] in the context of non-conformal brane holography. 2 This map has been used in the past to obtain the transport coefficients up to second order in the derivative expansion for blackfolds [30] and for the fluid dual to Rindler spacetimes [31], by mapping the corresponding quantities of the conformal fluid dual to large AdS black holes. Similarly, in an 1/D expansion, the quasi-normal frequencies of AdS black branes were shown to match under the map the unstable frequencies of Ricci-flat black branes [38]. These examples show the validity and effectiveness of the correspondence.
where we have decomposed the base space coordinates as y a = {x μ , r }. 3 Now, we add on both sides a general perturbation that depends on all coordinates, including the toroidal coordinates on AdS side and the spherical coordinates on the Minkowski side. The question we would like to answer is whether we can extend the AdS/RF map to apply to these perturbations.
To this end we will perform the dimensional reduction described above, but keeping this time the full towers of Kaluza-Klein (KK) modes. We will see that the resulting zero-modes are mapped into each other -this simply reflects the original AdS/RF map. We will however be more interested in the higher, massive modes, that deform the internal torus and sphere respectively. Naively there should be no way to map the single modes into each other: after all we are comparing KK modes on a torus to KK modes on a sphere! Surprisingly, in the limit the dimension of the compact space tends to infinity there is one-to-one correspondence between the modes. This paper is organised as follows. In the remainder of this section we discuss our conventions. In Sect. 2 we set up the two Kaluza-Klein reductions: we explain the KK decomposition of the perturbations and construct gauge invariant variables. Then in Sect. 3 we insert the KK decomposition in the field equations and derive the equations that the gauge invariant combinations satisfy. These equations are shown to follow from an action in Sect. 4. In Sect. 5 we decouple the equations, and we completely solve them in Sect. 6. In Sect. 7 we consider the large n and d limit and show that the AdS/RF correspondence maps individual modes to each other. We conclude in Sect. 8 with a discussion of our results. The paper contains two appendices: in "Appendix A" we discuss how the AdS/RF map acts on the zero modes and in "Appendix B" we provide a summary of the mathematical results on the harmonic decomposition of the sphere and torus.
Notation and conventions On the RF side of the correspondence we consider D = n + p + 3 dimensional spacetimes on which define coordinates X A , and use early capital latin letters A, B, … for tensor indices. We will use a bar for all quantities defined in these spacetimes, so the metric isḡ AB , the associated covariant derivative∇ A , and the d'Alembertian¯ .
We denote collectively X M the d + 1 coordinates on the AdS side of the correspondence, with the late capital latin letters M, N , … to mark tensor indices. Quantities defined on this manifold are denoted with a check sign, thus the metric These spacetimes undergo a KK reduction down to p + 2 dimensions, where we define coordinates y a , with early latin indices a, b, …. For the backgrounds we are interested in, these lower-dimensional manifolds are flat, and we define on them a Minkowski metric η ab , the partial derivative ∂ a , and the flat d'Alembertian = η ab ∂ a ∂ b . These coordinates are further decomposed as y a = {x μ , r }, with a holographic coordinate r , and p + 1 boundary (or brane) coordinates x μ , with greek indices μ, ν, …. On this boundary the induced metric is the Minkowski metric η μν . RF spacetimes are compactified over a (n + 1)-sphere S n+1 , on which we define coordinates θ i with indices i, j, … and its unit round metric σ i j . The covariant derivative operator on this sphere is given by D i , and the Laplace operator by θ . By convention, we raise and lower the sphere indices i, j, …using the sphere metric σ i j and its inverse σ i j , with σ i j σ jk = δ i k . Similarly, the AdS spacetimes are compactified over a (d− p − 1)-dimensional torus T d− p−1 , with coordinates χ i and indices i, j, …, that should be easily distinguished from the sphere indices by the context. The coordinates are identified with period τ that sets the size of the torus, χ i ∼ χ i + τ . Finally, on T d− p−1 , we have the flat metric δ i j , and the partial derivatives ∂ i .

Kaluza-Klein reductions
Our aim is to investigate whether it is possible to perturbatively unfreeze the compact manifolds in the AdS/RF map, i.e. we will start with an AdS/RF pair and ask whether we can map across perturbations that depend on the compact manifolds. We will discuss this in the simplest case where the pair is AdS on a torus/Minkowski on a sphere. To address this issue, we first need to analyze what are the possible perturbations. Thus, to start with, we need to perform a full KK reduction of vacuum Einstein gravity on a sphere, and a full KK reduction of AdS gravity on a torus.
To this end, we will first decompose the spacetime fields according to their transformation properties under diffeomorphisms of the compact spaces, and then expand them further into harmonics of the sphere and of the torus. We will then construct gauge invariant variables to make the KK reduction independent of any choice of gauge fixing. This can be done systematically, using the gauge invariant KK reduction technique developed in [44]. Armed with these variables, we can finally find the field equations that these KK modes must verify, in both reductions. We will see that it is possible to decouple and solve all equations. Discussions of such complete KK reductions are rare in the literature, see [45] for such an example and [46] for a review. As the techniques discussed here may be useful in different contexts, an effort was made to present a complete and self-contained discussion.
Vacuum Einstein gravity and deformations of Minkowski spacetime On the one side of the correspondence we have vacuum Einstein gravity in n + p + 3 dimensions, by which we simply mean General Relativity with no cosmological constant nor external matter. The equations of motion arē R AB = 0, so that the solutions are Ricci-flat manifolds. Its vacuum is Minkowski spacetime whose metric, in coordinate adapted to the Ansatz (1.4), is Here η μν is the ( p + 1)-dimensional Minkowski metric, and σ i j is the unit metric on the round S n+1 . Upon reduction on the sphere, we are left with a ( p+2)-dimensional theory with coordinates y a = {x μ , r }, and with its indices a, b, … being raised and lowered by convention with the Minkowski metric η ab . Perturbing the background metricḡ AB with a small perturbation h AB , we find that the resulting metricḡ + h solves the original field equations to first order in h AB if the perturbation solves the linearised Einstein equations where | indicates the covariant derivative∇ A compatible with the background metricḡ.

AdS gravity and deformations of AdS spacetime
On the other side of the correspondence we have AdS gravity in d + 1 dimensions, by which we mean General Relativity in presence of the negative cosmological constant (1.1) and no external matter fields. The field equations are thuš G M N + ǧ M N = 0. The vacuum solution in this case is given by AdS spacetime whose metric, in Poincaré coordinates, is given by Here r is the holographic radial coordinate of the Poincaré patch, and z α are the coordinates of its d-dimensional conformal boundary with Minkowski metric η αβ . To adapt this metric to Ansatz (1.2), we further single out d − p − 1 spacelike directions along the boundary, and split the coordinates as z α = {x μ , χ i }, The χ i coordinates are compactified on a torus T d− p−1 , with flat metric δ i j . The remaining p +2 coordinates y a = {r, x μ } describe again the theory obtained after dimensionally reducing, this time over the torus. The corresponding indices a, b, … are once again raised and lowered by convention with the Minkowski metric η ab . For the perturbed metricǧ + h to satisfy the AdS gravity field equations at linear order in the small perturbation h M N , the latter must solve the linearized Einstein equations where the extra term comes from the cosmological constant, and δ R M N is given by (2.2) with the backgroundḡ (and corresponding covariant derivatives) replaced byǧ.
AdS/RF correspondence for perturbations respecting the original Ansätze Let us pause before performing the full KK reduction to consider how the AdS/RF map acts on these perturbed solutions. When the perturbations respect the Ansätze (1.2) and (1.4), the map goes through in a straightforward way, and it is easy to see how the various components get mapped into one another. This is done in "Appendix A". From the KK perspective, these are the zero modes, that survive when we freeze the internal manifolds. We are instead interested in the fate of the massive KK modes, the ones that pull the metric away from Ansätze (1.2) and (1.4), and appear as soon as the internal manifolds are unfrozen. On these modes, we cannot directly apply the original AdS/RF map. Instead, we will perform a full KK reduction over the internal manifold on both sides of the correspondence, and then compare them to find out if the resulting modes are related in any way.

Harmonic decomposition of the fields
In order to perform the KK reductions, we first decompose the fields in scalar, vector and tensor components with respect to the reduced manifold, and expand them in harmonics of the compactification space. Thus, the perturbation of the Minkowski spacetime is expanded in spherical harmonics, while the expansion of the perturbation of AdS is simply a Fourier expansion.
Mode decomposition on S n+1 We can use the spherical symmetry of the metric Ansatz (1.4) to decompose the metric perturbation h AB (y a , θ i ) of Minkowski into scalar h ab , vectorial h ai , and tensorial h i j components under the rotation group SO(n +2). We further decompose the latter into a symmetric traceless part h (i j) and a trace part h i i . We then expand all these quantities into scalar spherical harmonics S I s (θ ), vector harmonics V I v i (θ ) and tensorial harmonics T . The latter form a complete set of eigenfunctions of the Laplace operator on the (n + 1)-sphere, with eigenvalues I s , I v , and I t respectively. Their definition, as well as some of their properties, can be found in "Appendix B.1". The resulting decomposition of the metric perturbation reads where D i are covariant derivatives compatible with the unit metric σ i j on S n+1 , and we are summing over repeated indices I s , I v , and I t that label the (scalar, vectorial, and tensorial respectively) representations of SO(n + 2). In the following, we will omit the summation signs and assume Einstein's convention for summing over repeated indices. Also, we will leave the coordinate dependence in fields and harmonics implicit. The metric perturbation is hence decomposed in the fields 4 , φ I s s , and π I s that depend on the coordinates (x μ , r ). The overall factors of r 2 in Eqs. (2.7)-(2.9) ensure that these fields transform covariantly in the reduced theory. From the point of view of 4 Note that the modeφ I t t carries a hat, while the others do not. The reason is that it is a gauge invariant mode, as we will shortly see. The same remark holds when applied to the AdS modeψ , φ I s s , π I s are scalar perturbations. When referring to scalar/vector/tensor modes, we will mean that from the perspective of the ( p + 2)-dimensional theory. In addition, we use parentheses to indicate symmetric traceless combinations on the tangent space to the sphere, so that the full tensorial part of the perturbation is given by (2.11) Finally, for convenience, we also define h I s as the trace of the KK gravitons, As last note, recall that S I s is a constant for l = 0, V I v a is defined for l ≥ 1 only, and T I t i j is defined for l ≥ 2 only. As a consequence, the coefficients B I v (v)a , B I s (s)a , and φ I s s appear in the expansion for l ≥ 1 only, and similarly the tensor modê φ I t t is present for l ≥ 2 only. Furthermore, as the l = 1 vector harmonics are the Killing vectors of S n+1 , D (i V 0 j) = 0 and the coefficients φ I v v exist only for l ≥ 2.

Mode decomposition on T d− p−1
The mode decomposition on the torus is essentially Fourier expansion. However, we will formulate the problem in a way that is close to what is done in the case of the sphere. We decompose the generic metric perturbation h M N (y a , χ i ) of AdS into scalar h ab , vector h ai , and tensor h i j components 5 with respect of the group of isometries of the torus T d− p−1 . We also split the tensor component h i j into a symmetric traceless part h (i j) and a trace part h i i . Then, the resulting components are further expanded in Fourier (harmonic) modes on that torus, 5 We use the same symbol for the components of Minkowski and AdS perturbations. We hope this will not lead to any confusion, since it will always be clear which case we are discussing, and the comparison of the two KK reductions will always be performed using the modes obtained from the harmonic expansion, which are easily differentiated by their notation.
2" together with some of its properties that we will use later. In the following, we will assume Einstein's convention for summing over the repeated indices m s , (k, m v ), and (k, l, m t ) that label the representations of the torus isometry group. Here m s , m v , and m t are the wave number vectors, and the Fourier modes are eigenfunctions of the Laplace operator on the torus with eigenvalues − m 2 s , − m 2 v , and − m 2 t respectively. The metric perturbation of AdS is hence decomposed in the fields h m s ab (KK gravitons), , ψ m s s , and m s (scalars) that depend on the coordinates y a only. The overall factors of 2 /r 2 in the definitions (2.13)-(2.16) ensure that these fields transform covariantly in the reduced theory. When referring to scalar/vector/tensor modes, we will mean that from the perspective of the ( p + 2)-dimensional theory. In addition, we have used parentheses to indicate symmetric traceless combinations on the tangent space to the torus, The full tensorial part of the perturbation is then given by Finally, for convenience, we also define h m s as the trace of the KK gravitons, Since the eigenmodes are constant when their eigenvalue −m 2 s vanishes, their derivatives vanish. Therefore the coeffi-cients C m s (s)a and ψ m s s appear in the expansion when m 2 s = 0 only, and

Gauge invariant variables
Not all the fluctuations are independent, as some modes are diffeomorphic to each other or to the background solution.
Indeed, under a change of coordinates the linearized perturbations transform as 6 where D A is the covariant derivative of the background metric. An analogous formula describes the change δh M N in the metric fluctuation of AdS spacetime. One could at this point fix a gauge and work in it, but that would be inconvenient when using the results on solutions that are not written in that gauge. We would rather eliminate this ambiguity, and we will therefore work using gauge invariant variables, following [44] where a systematic way to define them was presented. We first decompose the vector ξ A generating the diffeomorphism into its scalar components ξ a and its vector components ξ i with respect to the isometry group of the relevant compactification manifold, and expand them in harmonics. Then we calculate how the perturbation modes vary under such diffeomorphisms. The crucial observation is that one can build linear combinations of the perturbation modes (and their derivatives) that are pure gauge, and whose variation under the diffeomorphism yields precisely the components of ξ . They can be used to compensate for the variations of the metric perturbation under diffeomorphisms, and thus construct gauge invariant variable. Let us now see in more detail how that works.

Gauge invariant variables at linear order for fluctuations of Minkowski Expand the diffeomorphism generator ξ
It is easy to check that the metric perturbations varies, to linear order, according to 6 In general the right hand side of (2.21) contains terms which are higher order in fluctuations. The leading order terms displayed in (2.21) are sufficient for deriving the gauge invariant combinations of linearized fluctuations, see [44] for a complete discussion.
We see thatφ I t t is invariant under this transformation. On the other hand, φ I s s and φ I v v are pure gauge field, and they can be complemented by an additional pure gauge fieldB I s (s)a given bỹ It is straightforward to check that the hatted fieldsĥ I s ab ,B I v (v)a , φ I t t , andπ I s account for all the physical degrees of freedom of the metric perturbation, and that they are not affected by diffeomorphisms, Note however that, as explained in Sect. 2.1, the modes B I v (v)a , B I s (s)a , and φ I s s appear in the expansion in spherical harmonic for l ≥ 1 only, and the modes φ I v v andφ I t t for l ≥ 2 only. As a consequenceB I v (v)a is only defined for l ≥ 2 and we have to work with the unhatted variable B I v (v)a when l = 1. The latter field transforms nevertheless as a gauge field from the perspective of the ( p + 2)-dimensional theory, (2.31) Actually, these gauge fields are the SO(n + 2) gauge fields related to the isometry of the sphere S n+1 , but here we only see the linear part of the gauge invariance. Similarly,B I s (s)a can only be defined for l ≥ 1, and one has to work with the unhatted h I s ab and π I s fields when l = 0.
Specializing to these cases, these transform as The π 0 perturbation just amounts to a redefinition of the radial coordinate and may be set to zero by a radial diffeomorphism, and h 0 ab transforms as a metric, as it should.
Gauge invariant variables at linear order for fluctuations of AdS The same approach can be applied to perturbations of the AdS metric.
It is convenient at this point to fully exploit the Poincaré symmetry of the background metric (2.3), and combine, for the purpose of this calculation, the coordinates into so that the background metric becomes ds 2 = ( 2 /r 2 )η mn dζ m dζ n and we can use the (d + 1)-dimensional Minkowski metric η mn to raise and lower indices. Then the variation (2.21) of the metric perturbation assumes the compact form from which we can read off how the modes change under this transformation, Again, we find that the scalar modeψ that transforms under diffeomorphisms as δC m s (s)a = ξ m s a . As before, we use these pure gauge fields to compensate for the variations of the remaining modes by defining the gauge invariant fieldsĥ m s ab , Supplementing these with the scalar modeψ , andˆ m s that describe metric perturbations of AdS, As explained earlier, the coefficients C m s (s)a , ψ m s s , and ψ (k,m v ) v appear in the Fourier expansion only when the corresponding eigenvalue is non-vanishing. As a consequencẽ C m s (s)a (and the hatted fields) can be defined for m 2 s = 0 only, and one has to work with the unhatted fields h m s ab , m s , and ) when dealing with zero modes. Restricting to zero modes the gauge transformations read, where D a is the AdS covariant derivative. We will see later on that C (k,0) (v)a satisfies Maxwell equations in AdS. These are linearized modes corresponding to the d − p − 1 KK vectors (corresponding to an off-diagonal reduction) that one may turn on when we Kaluza-Klein reduce over a torus. The 0 perturbation just amounts to a redefinition of the radial coordinate and may set to zero by a radial diffeomorphism, and h 0 ab transforms as a metric, as it should.
A note on the De Donder-Lorentz gauge To perform the Kaluza-Klein reduction it is common to fix the gauge by imposing the De Donder-Lorentz (DDL) gauge fixing condition on the perturbations, In the case of the dimensional reduction of Einstein vacuum gravity on a sphere, this gauge condition kills the components , and φ I s s , leaving us with the simpler decomposition Similarly, when reducing AdS gravity on a torus, the DDL condition kills the components , and ψ m s s , so that (2.47) One could thus work directly in the De Donder-Lorentz gauge and then, at the end of the computation, relax it by adding a hat to all quantities in order to obtain the expressions for the gauge invariant quantities. We will however not impose this gauge, but rather work with gauge invariant perturbations, as the cancellation of all gauge dependence is a useful consistency check.

Equation of motion for Kaluza-Klein modes
In this section we derive the field equations that the Kaluza-Klein modes satisfy by substituting the KK expansion in the linearized field equations.

Perturbations of Minkowski reduced on a sphere
We first decompose the linearized field Eq. (2.2) into their scalar ab, vector ai, and tensor i j components under the rotation group of the sphere. After evaluating all covariant derivatives on the background metric (2.1), one obtains Next, we project these equations on our basis of spherical harmonics of S n+1 and rewrite all fields in terms of the hatted, gauge invariant fields. The scalar equation becomes simply The projection of the vector components gives and finally the projection of the tensor components yields As expected, all gauge dependence cancels out.
Special cases When l = 0, S I s is constant, and its derivatives vanish. Hence, the perturbations that respect the S n+1 are described by the fields h l=0 ab and π l=0 . These fields verify the two equations E 2r ∂ a h ar − r ∂ r h a a + 2nh rr − r 2 π + 2(n + 1) r ∂ r π + 2n r 2 π = 0. (3.12) The other field equations, such as the linear relation between the scalarsĥ I s andπ I s , only hold for l > 0. When l = 1, V I v i is a Killing vector and D (i V I v j) = 0, and the modes φ I v v do not exist. In this case we get (3.5) but witĥ  14) and this equation is manifestly gauge invariant under Independent equations There are linear differential relations between the field equations for these modes, Therefore only E i j D (i D j) S Is = 0, can be deduced from them. Note however that the latter are obtained with a I s prefactor; this was expected, as these equations hold for the I s = 0 modes only. The fact that there is linear dependence between the field equations is due to gauge invariance: the fields B I s (s)a , φ I v v and φ I s s are pure gauge. This will become obvious in the Lagrangian analysis in Sect. 4.

Perturbations of AdS reduced on a torus
Since the Poincaré metric is conformal to the Minkowski metric, it is quicker to evaluate the linearized Eq. (2.5) for a small metric perturbation introducing once more the coordinates ζ m = {r, z α } = {r, {x μ , χ i }} and working with the background metric ds 2 = ( 2 /r 2 )η mn dζ m dζ n , using the (d+1)-dimensional Minkowski metric η mn to raise and lower indices. The resulting equations can be written as E ( ) mn = 0, where Decomposing the ζ m coordinates in the holographic radial coordinate r and boundary coordinates z α -in which the background metric assumes the form (2.3) -the linearized field equations become, Since the metric η αβ is flat, it is trivial to further decompose these coordinates into boundary coordinates x μ and torus coordinates χ i , and then combine them with the radial coordinate r to form y a = {r, x μ } as usual. Next, we project these equations on the Fourier basis of the torus T d− p−1 , and rewrite all fields in terms of the hatted, gauge invariant fields. The scalar equation becomes simply The projection on the vector modes gives and finally the projection on the tensor modes yields The other field equations, such as the linear relation between the scalarsĥ m s andˆ m s , only hold for m 2 s > 0. This is analogous to what happens for Minkowski perturbations. When i is a constant: we need to work with the unhatted variable C (k,m v ) (v)a , and (3.26) does not hold. Defining the associated field strength Independent equations There are linear differential relations between the field equations for the scalar modes, and E ( ) i j ∂ (i ∂ j) S ms = 0, can be deduced from them. Note however that they are obtained with m 2 s prefactors; this was expected, as the latter equations hold for the m 2 s = 0 modes only. Again, these extra equations are a consequence of the gauge freedom that allows to choose arbitrary fields C m s (s)a and ψ m s s . This will become obvious in the Lagrangian analysis of next section.

Quadratic action for the perturbations
We start with the Einstein-Hilbert action in presence of a cosmological constant, We consider perturbations h AB on top of a backgroundǧ AB solving the field equations, g AB =ǧ AB + h AB , and expand the action up to quadratic order in the perturbation. The inverse metric is given to this order by where we use the background metricǧ AB to raise/lower indices. Expanding the measure we obtain, while the Ricci tensor can be expanded as withŘ AB the Ricci tensor of the background spacetime and its linear and quadratic variations given respectively by [44] R (1) where ∇ A is the covariant derivative associated to the background metricḡ AB , and we have defined Then, the action at quadratic order can be written as This action can be rewritten in terms of the perturbation h AB using Eqs. (4.5)-(4.7), and after a few integration by parts simplifies to The result for quadratic expansion in the case of zero cosmological constant can be obtained from (4.9) by setting = 0 and replacingǧ byḡ: (4.10)

Quadratic action for the perturbations of Minkowski
Let us start by writing down the quadratic action (4.10) for Minkowski perturbations respecting the symmetries of the sphere. For such perturbations, we take all fields to be independent of the coordinates on the sphere and set (4.11) These perturbations will be discussed in "Appendix A". To avoid clutter we drop the index 0 from h 0 ab (and h 0 (ab) , H 0 ). Then the quadratic action (4.10) reduces to, (4.12) Here we performed the trivial integration on the S n+1 , and an integration by part to get rid of the π∂ r π term. It is easy to check that the variation of this action with respect to h ab and π gives the correct field equations for these perturbations.
It is an instructive exercise to express this action in terms of the fields (h (ab) , H, π): (4.13) Again, one can check that by varying this action with respect to the fields (h (ab) , H, π), one recovers the correct field equations, but -more interestingly -one can also define a conserved current J a given by 14) The conservation of this current, ∂ a J a = 0, is essentially equivalent to the field equation obtained by varying the action with respect to the field H . This is expected: the isometries of the compact space give rise to global symmetries in the reduced theory, and the momentum constraint becomes the conserved current. After this warm up exercise, we are ready to compute the full quadratic action for Minkowski perturbations. We work with the background metric (2.1) and decompose the fields in harmonics of the S n+1 using (2.6)-(2.9). We also impose the De Donder-Lorentz gauge ( where we have introduced the field strengthĜ I v (v)ab associated to the vector fieldB I v (4.16) and the constants S m s t , V m v t , and T m t t are defined by (4.17) We can check that this action yields the correct field equations for the perturbations of Minkowski spacetime. First, the variation δφI t t S 0 of the action with respect to the fieldφ The other equations are not independent, and follow from varying the action S 0 with respect to B I s (s)a , φ I s s , and φ I v v , after expressing the gauge invariant combinations in terms of the original fields. One can indeed check that the variation = 0, and that the variation with respect to φ I s s and B I s (s)a , give the other equations Taking the variation with respect to the field h mn , and subtracting from the result η mn /(d −1) times its trace, one recovers precisely Eq. (3.18) for the metric perturbations of AdS spacetime. We further decompose the metric perturbation h mn in its scalar, vector, and tensor components with respect to the group of isometries of the torus, and expand them in Fourier modes on T d− p−1 , according to (2.13)-(2.16). Then, integrating over the torus, we to obtain the ( p + 2)-dimensional reduced action. Also, we work in De Donder-Lorentz gauge  (4.23) and we use the notation H m s = η abĥms ab (4.24) for the trace of the ( p + 2)-dimensional metric perturbation. Then, the resulting action is (4.25) where the constants S m s t , V m v t , and T m t t are defined by On the other hand E = 0 is not an independent equation; it follows from E , and m s . Then, the variation with respect of the pure gauge field ψ (k,m v ) v yields (using the definition (2.41) and applying the chain rule), The resulting equation is actually first order in derivatives and agrees precisely with E = 0. Likewise, by asking the stationarity of the action with respect to the fields ψ m s s and C m s (s)a , we obtain other differential operators acting on the field equations. These will simplify the field equations (reducing the order in derivatives), to give the relations E Notice that the action (4.25) is valid also when m 2 v = 0. In this case one should drop the hat fromF

Decoupling the Kaluza-Klein equations
In this section we look closely at the structure of the Kaluza-Klein equations, both for perturbations of Minkowski and for perturbations of AdS, and show that we can decouple them (almost) completely.

Perturbations of Minkowski spacetime reduced on S n+1
The field equations for the metric perturbation modes of Minkoswki are obtained in Sect. 3.1. First, we notice that the scalar modeφ I t t , associated with a tensor harmonic with eigenvalue I t given by (B.5), decouples from all the other fields. Its equation of motion, given by (3.7), is given by The vector modeB I v (v)a decouples from the rest of the system as well: its equation of motion is given by Eq. (3.5) and reads where we used the field strengthĜ I v (v)ab associated to the vector fieldB I v (v)a , defined in (4.16). When l ≥ 2 this vector must additionally satisfy Eq. (3.8). It is the divergenceless condition that is however not independent from the previous field equation, as can be seen by comparing the equation obtained from (5.2) by acting with ∂ b on it with the equation obtained by setting b = r in it. When l = 1, Eq. (5.2) still holds but for unhatted variable B I v (v)a , and equation (5.3) does not hold anymore (but we have an additional gauge invariance).
The remaining modes,ĥ I s ab andπ I s , are associated with scalar harmonics. First of all we notice that the trace modê h I s is proportional to the trace mode on the sphereπ I s by equation E In order to do this consistently, we need to decompose the metric perturbationĥ I s ab into its traceĥ I s and its symmetric traceless partĥ I s (ab) , The remaining coupled equations for these modes are given by E (0) ab S Is = 0, E (0) ai D i S Is = 0, and E (0) i j σ i j S Is = 0 7 The n = 1 case is special because we are reducing over a twosphere, on which there are no tensor harmonics. Therefore, there is no fieldφ I t t . Furthermore, the traceĥ Is is automatically vanishing by Eq. (5.4). Correspondingly, the dependence on Is of theπ Isπ Is term in the action (4.15) drops out.
[see respectively (3.4), (3.6), and (3.10)]. The second of these equations is not independent from the others, but it can be used -together with its divergence -to eliminate the divergences ∂ aĥ I s ab and ∂ a ∂ bĥ I s ab from the other two field equations. Finally, we introduce a new scalar fieldφ I s defined bŷ The third Eq. (3.10) and the rr component of the first one (3.4) become respectively,   associated with a tensor harmonic decouples from the other fields, and must solve the equation The vector modeĈ decouples as well from the rest of the system. Its equation of motion is given by Eq. (3.23) and reads (v)ab is the field strength associated to the vector fieldĈ (v)a , as defined by (4.23). When m 2 v = 0 this vector must additionally satisfy Eq. (3.26) that imposes the vanishing of its divergence, This condition is however not independent from the previous field equation, as can be seen comparing the equation Following the Minkowski steps, we decompose the metric perturbationĥ m s ab into its traceĥ m s and its symmetric traceless partĥ m s (ab) , i j δ i j S ms = 0 (see respectively (3.22), (3.24), and (3.27)). Again, the second of these equations is not independent from the others, 8 When d − p − 3 = 0, we are reducing over a two-torus, on which there are no tensor harmonics. Therefore, there is noψ (k,l,m t ) t field in that case. Moreover, the traceĥ ms of the perturbation vanishes by Eq. (5.15). Analoguously, the m 2 s -dependence of the coefficient of thê msˆ ms term in the action (4.25) drops when d − p − 3 = 0. and we use it -together with its divergence -to eliminate the divergences ∂ aĥ m s ab and ∂ a ∂ bĥ m s ab from the other two field equations. The resulting equations can be completely decoupled by defining the new fieldsφ m s andχ m s as (the transformation is invertible as long as d = 2), and a new symmetric fieldh m s (ab) that is both stripped from its trace and its rr component (i.e. it is such that η abh m s (ab) = 0 andh m s (rr) = 0) aŝ Using these fields, the complete set of field equations for the scalar modes becomes While the second order wave equations forφ m s ,χ m s , and h m s (ab) are completely decoupled (contrary to what happens for the corresponding equations for Minkowski on a sphere), some coupling between these fields survives in the last two equations, that are valid for m 2 s = 0 and descend from Eq. (3.24).

Solving the Kaluza-Klein equations
In this section we solve the Kaluza-Klein equations for linearized metric perturbations for both Minkowski and AdS.

Solving for Minkowski perturbations
We first solve Eq. (5.1) for the linearized scalar perturbation φ I t t associated with tensor harmonics of S n+1 , This is a separable equation; the radial part of the modes solve a Bessel equation in r , and the dependence in the remaining 'brane' directions x μ satisfies a D'Alembert equation. The latter is therefore solved by Fourier modes e ik·x , where we use the notation k · x for the contraction of the momentum along the brane directions k μ with the coordinates x μ . The general solution is thus a superposition of the modeŝ where J l+ n 2 is a Bessel function of the first kind and Y l+ n 2 is a Bessel function of the second kind. Here φ 1 and φ 2 are integration constants, and we used I t = −l(l + n) + 2 and k 2 r = −k 2 . k r may be thought of as a radial momentum which can be combined with k μ to form the ( p + 2)-dimensional momentum k a . The equations of motion require then that the vector k a is null, k a k a = k 2 r + k 2 = 0. As we will see, the solutions of all perturbation equations are linear combinations of Bessel functions of the first and second kind. To simplify the presentation, the integration constant associated with J Bessel functions will always carry an index 1 and those associated with Y Bessel function an index 2. Then if we know the part of the general solution that depends on J Bessel functions, we can obtain the part that depends on Y Bessel functions by simply replacing the J Bessel functions by the Y ones and change the index of the integration constants from 1 to 2. Then instead of presenting the solutions as in (6.2), we will usê All solutions in this and the next subsection will be presented in this way. Next we discuss the vector perturbationsB I v (v)a . They satisfy Eqs. (5.2) and (5.3), reproduced here for convenience, with the field strengthĜ I v (v)ab defined in (4.16). These equations hold when l > 1. We will return to the l = 1 case below. Taking the radial component a = r in (6.4) and using (6.5), we obtain a decoupled equation forB I v (v)r , This is the same equation as (6.2) and thus the general solution iŝ where the momentum k a = {k r , k μ } is null, and b I v 1 , b I v 2 are integration constants. Note that in (6.7) and in all similar equations in the rest of this section we will suppress indices such as I v to avoid clutter. The equation for the remaining components is obtained by setting a = μ in (6.4), and using (6.5) to eliminate the r -derivatives ofB I v (v)r , The general solution to the homogeneous part of this equation readŝ (6.9) Here β 1 μ and β 2 μ are two arbitrary polarization vectors. We further need a particular solution to Eq. (6.8). Here and in the rest of this section we will assume that k r = 0. When k r = 0, both in the Minkowski and the AdS cases, the ODE's become of the Euler type and can be integrated by elementary means (including finding all particular solutions). The particular solution for (6.8) is given by 9 with ε μ an arbitrary constant vector. We use this freedom to simplify the solution of the divergence Eq. (6.5). Then, given 9 This result is obtained using the following general results. If f satisfies where a is a constant, then (6.12) a solutionB I v (v)r determined by b 1 and b 2 , as given by (6.7), the general solution to the full equation forB I v (v)μ is given bŷ 14) wherê (v)r = 0, and the general solution is the homogeneous solution (6.9) (for the unhatted variable) with arbitrary polarization vectors β 1 μ and β 2 μ , Gauge invariance may be used to make the polarization vectors transverse, (6.16).
We finally need to deal with the perturbations associated with scalar harmonics of S n+1 , namely the scalar perturbationπ I s and the tensor perturbationĥ I s ab . We have partially decoupled the equations they satisfy by introducing the scalar fieldφ I s in Eq. (5.6), resulting in Eqs. (5.7) and (5.8), that we report here once more for convenience, Contracting with η μν and using η μνĥ I s (μν) = −ĥ I s (rr) (which follows from η abĥ I s (ab) = 0) results in an equation which involves onlyφ I s , which automatically holds as a consequence of (6.18). Finally, the solution to (6.26) is constrained by equation (5.10), We now solve these equations. The homogenous solution of (6.24) iŝ where h 1 μ and h 2 μ are two constant ( p + 1)-vectors, and k a k a = k 2 r + k 2 = 0. A particular solution is given by 11 Using (6.20), we find that the solution of (6.24) is given bŷ We now turn to (6.26). Its homogenous solution iŝ where h 1 μν and h 2 μν are constant symmetric traceless ( p + 1)tensors and k a k a = k 2 r + k 2 = 0. The particular solu- 11 Actually, rφ Is solves the homogeneous equations, so its coefficient may be chosen at will. The choice in (6.29) simplifies the solution of (6.25). tion 12 is a linear combination of r −n/2 {r J 1+l+ n 2 , rY 1+l+ n 2 , r 2 J l+ n 2 , r 2 Y l+ n 2 }. Altogether we havê wherê  12 Consider the differential operator (6.34) it satisfies the identities L r 1− n 2 J l+ n 2 +1 (k r r ) = 2k r r −n/2 J l+ n 2 (k r r ), (6.35) L −k r r 2− n 2 J l+ n 2 (k r r ) + 2(l + n 2 + 1)r 1− n 2 J l+ n 2 +1 (k r r ) = 4k 2 r r 1−n/2 J l+ n 2 +1 (k r r ), (6.36) that can be used to obtain the particular solution.
−η μν k 2 r 2 ϕ 1 J l+ n 2 (k r r ) (6.41) where, for s = 1, 2, is indeed a Bessel equation in the radial direction, and is solved by separation of variables: its general solution is given by the superposition of modeŝ (k a k a = −m 2 t ), (6.44) with ψ 1 , ψ 2 integration constants. Again, k · x denotes the contraction of the boundary components k μ of the wave vector with the p + 1 boundary coordinates x μ , and we define the ( p +2)-dimensional wave vector k a = {k r , k μ }. Contrary to what we obtained for Minkowski perturbations, the wave vector for AdS perturbations is massive, with mass set by the eigenvalue m 2 t . We next move to the vector modes. They satisfy Eqs. (5.13) and (5.14), These are decoupled equations that are easily solved in terms of Bessel functions. Equation (6.48) is identical with (6.43) and thus is solved in the same way, while the extra term in (6.47) simply shifts the order of the Bessel function: with γ 1 , γ 2 arbitrary constants andγ 1 μ ,γ 2 μ arbitrary polarization vectors. Again, the wave vector is timelike, k a k a = k 2 r + k μ k μ = −m 2 v . We are not done yet, as we must additionally impose the second Eq. (6.46).
This divergence equation is only present when m 2 v = 0, and in that case it imposes constraints between the integration constants.
On the other hand, when m 2 v = 0 the divergence Eq. (6.46) is not present; instead there is a gauge invariance that can be used to set C (k,m v ) (v)r = 0. Thus, the general solution is simply given by (6.50) with a null momentum k a , k a k a = k 2 r + k μ k μ = 0.
(6.52) and one can use the gauge invariance to impose k μ γ 1 μ = k μ γ 2 μ = 0. We finally turn to the perturbations associated with scalar harmonics,χ m s ,φ m s , andh m s (ab) . We have already decoupled completely the equations that govern them, obtaining the system of Eq. (5.19). The equations for the scalarsχ m s andφ m s , are separable and are easily solved by using Bessel functions in this section. These different behaviors are a direct con-Finally, one may match the integration constants of the scalars associated with tensor harmonics, φ s = ψ s . (7.15) We have thus succeeded in mapping all perturbations mode by mode in the large d and n limit, Starting from the next-to-leading order in the large d/n, the map becomes more complicated because the eigenvalues l and m enter in the expansion coefficients.

Discussion and outlook
In this paper we performed a Kaluza-Klein reduction of Minkowski over a sphere and of AdS over a torus. In the case of Minkowski the sphere was the celestial sphere transverse to a flat p-brane located at the origin of Minkowski and in the case of AdS the torus compactified part of the boundary directions. The reason for considering these two cases is that this is the simplest example of an AdS/RF pair, and we wanted to investigate whether one can perturbatively relax the restrictions that enter the construction of the AdS/RF map, namely the existence of a sphere on the Ricci-flat side and of a torus on the AdS one. Thus we allowed for general perturbations that depend on all coordinates, including those on the sphere and the torus, and asked if these perturbations can be mapped to each other via the AdS/RF map.
To address this question we constructed the most general perturbations by KK expanding around the background solution (Minkowski and AdS), keeping all massive KK modes. Such computations are rare in the literature and we hope that the streamlined discussion we present here will be useful more generally, in other contexts.
Usually KK reductions involve spacetimes that are direct products of a non-compact spacetime with a compact manifold, such as Minkowski × torus or AdS × sphere. In our case, the background solutions were warped products, and the torus (sphere) was on the AdS (Minkowski) side. It is also worth mentioning that on the Minkowski side all dimensions are non-compact: the sphere of the reduction arose from writing an Euclidean space in spherical polar coordinates.
When considering perturbations around background solutions, there is an intrinsic ambiguity in that there are diffeomorphisms that map perturbations to the background solu-tion or to each other. In most of the past literature, this issue was dealt with by imposing gauge fixing conditions. This is fine for the computation of the spectrum, but if one wants to use these results more generally (for example for mapping solutions to other solutions, as we want to do here) a better approach is to construct gauge invariant variables. We construct such gauge invariant variables for both reductions following the methodology developed in [44]. This provides a (non-trivial) example of the effectiveness of this method, which we believe should be useful in all problems were gauge invariant variables are needed.
We performed both reductions in parallel to emphasize their similarity. The equations of motion for the KK modes can then be obtained by substituting the KK decomposition in the higher dimensional field equations and then projecting on harmonics of the torus and sphere. Not all equations obtained in this fashion are independent, and this reflects the existence of the gauge transformations discussed in the previous paragraph. The same equations also follow by varying the action obtained by substituting the KK decomposition in the higher dimensional actions and integrating over the torus and sphere.
Remarkably, for the two reductions we performed, one can solve all perturbation equations in closed form. In the case of AdS, the equation for the perturbations reduce to a set of homogeneous Bessel equations that can be readily integrated (plus a few additional equations that impose relations among the integration constants). In the case of Minkowski, the perturbation equations are organized in a number of decoupled blocks. Within each block the equations take a nested form, with up to three layers: at the centre there are decoupled modes that satisfy homogenous Bessel equations; these modes then provide inhomogeneous terms for the ODEs satisfied by the modes at the next layer, which themselves provide inhomogeneous terms for the modes at the last layer. We were able to integrate all equations and obtain the general solution as linear combination of Bessel functions.
Having succeeded in finding the general solution of linear perturbations, we can then turn to the original question about the AdS/RF correspondence. Rather strikingly, the AdS/RF map acts mode by mode in the limit where the dimension of the sphere and torus goes to infinity. We will discuss how general linear perturbations are mapped by AdS/RF in a sequel to this paper [43]. There we will make a use of the opposite limit, namely the limit where either the sphere or the torus disappears, and we will formulate mathematical conditions for the existence of an AdS/RF map at the non-linear level.
We finish this paper with a few remarks about holography. On the AdS side, our results can be used to compute holographically the 2-point functions of a class of operators for the QFT obtained by putting a d-dimensional CFT on torus. Putting the CFT on a torus breaks conformal invariance, but the resulting theory is still constrained by the fact that the parent theory is conformal. The relevant QFT operators are the operators obtained by dimensional reduction of the CFT energy momentum tensor on the torus, keeping the entire KK towers.
Starting from the explicit solutions we obtained, one can extract the 2-point functions from their asymptotics using the methodology in [42]. For the zero modes, we have already done this computation in Sect. 2.2.1 of [31], and it would be interesting to work out the details for all KK modes. These the 2-point functions should be related to the 2-point function of a d-dimensional CFT energy momentum tensor (which is universal) via dimensional reduction. It is well known that conformal 2-point functions are related holographically to Bessel functions, and this explains why the solutions to the AdS perturbation equations are given by Bessel functions.
Via the AdS/RF correspondence, these results would then provide a holographic dictionary for Minkowski perturbations, which is particularly simple in the case of large n. It would be interesting to extract the physics implications of this. We only make a couple of remarks here. First, the AdS/RF map explains why the solutions to the Minkowski perturbations are Bessel functions, as it links these perturbations to those of AdS, which are given in terms of Bessels due to the underlying conformal structure of AdS. Second, we note that the AdS/RF correspondence maps asymptotic flatness to regularity in the interior of AdS and regularity in the interior of Minkowski to normalizable solutions in AdS [31]. It would be interesting to further develop this holographic dictionary.
where l, the degree, specifies an irreducible representation of the rotations group. S I s (θ ) are the scalar spherical harmonics and I s = (l, m i ) is a set of quantum numbers (including l) that labels uniquely the basis elements of the representation. The vector spherical harmonics V I v i (θ ) have n independent components and are hence non trivial for n ≥ 1. Finally, the tensor spherical harmonics T I t (i j) (θ ) are symmetric and traceless in the sphere indices, have (n − 1)(n + 2)/2 independent components, and are hence non trivial for n ≥ 2. It is also worth mentioning that S I s is constant when l = 0, so terms involving its derivatives should not be taken into account when considering the s-wave. Moreover, V I v i are Killing vectors of S n+1 when l = 1, so D (i V I v j) = 0, and the harmonic expansion contains terms proportional to D (i V I v j) = 0 only for l ≥ 2.
These form a complete set for functions on the sphere. Any scalar function can be written as a linear combination of the scalar harmonics S I s ; vector functions on the sphere can be expanded in vector harmonics V I v i and derivatives D i S I s of scalar harmonics; finally, symmetric traceless rank two tensors on the sphere can be expressed as a superposition of tensor harmonics T I t (i j) and derivatives D (i V I v j) and D (i D j) S I s of vector and spherical harmonics. This leads to the decomposition (2.6)-(2.9) for perturbations of Minkowski spacetime.
To conclude, we display a few properties of the spherical harmonics that we used to simplify the calculations, and can be easily obtained using the identities (B.2), given by the constant symmetric traceless tensors, T (k,l,0) (i j) = 1 2 δ k i δ l j + δ l i δ k j − 1 N δ i j δ kl , k ≤ l. It is worth remembering that when m 2 s = 0, m 2 v = 0, or m 2 t = 0 the corresponding modes are constant and their derivatives vanish.
Since the torus is flat, derivatives commute and we have also . (B.16) Finally, the following relations turn out to be useful,