Holographic OPE Coefficients from AdS Black Holes with Matters

We study the OPE coefficients $c_{\Delta, J}$ for heavy-light scalar four-point functions, which can be obtained holographically from the two-point function of a light scalar of some non-integer conformal dimension $\Delta_L$ in an AdS black hole. We verify that the OPE coefficient $c_{d,0}=0$ for pure gravity black holes, consistent with the tracelessness of the holographic energy-momentum tensor. We then study the OPE coefficients from black holes involving matter fields. We first consider general charged AdS black holes and we give some explicit low-lying examples of the OPE coefficients. We also obtain the recursion formula for the lowest-twist OPE coefficients with at most two current operators. For integer $\Delta_L$, although the OPE coefficients are not fully determined, we set up a framework to read off the coefficients $\gamma_{\Delta,J}$ of the $\log(z\bar{z})$ terms that are associated with the anomalous dimensions of the exchange operators and obtain a general formula for $\gamma_{\Delta,J}$. We then consider charged AdS black holes in gauged supergravity STU models in $D=5$ and $D=7$, and their higher-dimensional generalizations. The scalar fields in the STU models are conformally massless, dual to light operators with $\Delta_L=d-2$. We derive the linear perturbation of such a scalar in the STU charged AdS black holes and obtain the explicit OPE coefficient $c_{d-2,0}$. Finally, we analyse the asymptotic properties of scalar hairy AdS black holes and show how $c_{d,0}$ can be nonzero with exchanging scalar operators in these backgrounds.


Introduction
The AdS/CFT correspondence establishes an insightful routine to investigate a strongly coupled conformal field theory (CFT) by using appropriate weakly coupled gravity in antide Sitter (AdS) spacetime and vice versa [1]. Originally, the AdS/CFT correspondence is typically referred to as the duality between type IIB superstring in AdS 5 × S 5 and N = 4, d = 4 super Yang-Mills theory. The holographic principle is expected to be more general and can apply to a variety of gravity theories even without supersymmetry, and indeed it has passed a large amount of tests at the AdS scale, i.e. the locality holds at the scale that is never shorter than the AdS radius ℓ [2]. The results include the correct structures of two-point functions, three-point functions [3,4], conformal anomalies [5,6] in CFTs that are fixed by the virtue of conformal symmetry. Typically, even though the structures are the same, different gravity theories may lead to different CFT data. Thus gravities can be served as effective CFTs. By finding relations and bounds from the holographic CFT data that follow exactly the same pattern regardless of the specific details of a gravity theory, some universal properties of CFTs can be revealed. Known examples include the controlling pattern of shear-viscosity/entropy ratio and entanglement entropy by central charges [7][8][9][10], central charge relations [11][12][13].
Below the AdS scale where the higher-point correlation functions (≥ 4) come out to be visible, the generality of AdS/CFT becomes highly nontrivial. Fortunately, it was argued that any large N CFT with a parametrically large conformal dimensions for single-trace higher spin operator (spin J > 2) can have a weakly coupled gravity dual [2]. With this generality in mind, it is then natural to follow the same logic for the AdS-scale holography to find universal properties of CFTs by studying generic gravity theories.
The simplest case is the four-point functions. Typically, the four-point functions can be decomposed into conformal blocks which are completely determined by conformal symmetry with theory dependent OPE coefficients. (See [14][15][16] and also Appendix A for a brief pedagogical review.) One may then expect to study the four-point functions from the bulk to recover the conformal blocks and read off the OPE coefficients, and investigate some possible universal pattern. However, although the holographic conformal blocks as the geodesic Witten diagram were studied extensively in literature (here is the incomplete list [17][18][19][20][21][22][23],) explicitly computing them for quite general classes of higher-derivative gravities is rather challenging. The issue can be greatly simplified by considering the special case of heavy-light four-point functions in the heavy limit [24]. In this case, the four-point function can be treated as the two-point function of the light operators under overwhelmingly heavy states that can be viewed as black hole backgrounds in the bulk. This special case avoids the difficult task for addressing the holographic conformal blocks of four-point functions directly.
Focusing on the pure gravity black holes and deriving the holographic OPE coefficients, Ref. [24] found that the lowest-twist OPE coefficients for multi-stress tensors are universal.
We shall review this in section 2.
On the other hand, higher-point correlation functions, such as four-point functions of strongly coupled CFT can be studied further than the structures without referring to any specific theory by bootstrap program. (See [25] for a recent review.) The consistency conditions emphasized in bootstrap program, for example, the unitarity [26,27], the crossing symmetry [28][29][30][31][32] and averaged null energy condition (ANEC) [33][34][35], can universally constrain the spectrum and CFT data beyond two and three-point functions. These strong constraints in CFTs shall, inversely, be mapped to the constraints to the bulk theories to select those consistent (quantum) gravities with sensible CFT duals. For example, the crossing equation was used to restrict the interaction terms for bulk gravity theories [2].
Of course, the simplest consistency condition in CFT should be that the stress tensor is traceless. This implies in particular that the OPE coefficient c d,0 must vanish when the CFT does not have an additional scalar operator of conformal dimension d. Indeed it was verified [24] that c 4,0 = 0 from pure gravity black holes. In this paper shall verify the consistency for general c d,0 .
The main motivation of this paper is to study the holographic OPE coefficients for general black holes involving matter fields. We find that the patterns of lowest-twist OPE coefficients becomes more interesting, and the universality in CFT should be reconsidered.
The paper is organized as follows.
• In section 2, we begin with a review of the proposal for the heavy limit of holographic heavy-light scalar four-point functions and the corresponding holographic OPE coefficients. We review the construction and conclusions of [24] for pure gravity backgrounds in some detail. Moreover, we verify the consistency that the OPE coefficient c d,0 associated with the trace of stress tensor does vanish for general d. This fact motivates us to consider black holes with matters such that more primary operators can engage in, for instance, contributing to c d,0 = 0.
• In section 3, we consider AdS black holes charged under a Maxwell field in a general class of high-derivative gravity-Maxwell theories. In addition to the stress tensor, we find that the conserved current operator can also appear in the conformal blocks.
Some explicit low-lying examples in d = 4 and d = 6 are presented to gain insights.
Moreover, we obtain a recursion formula for computing the OPE coefficients involving at most two currents in general even dimensions d. We find some clear patterns in the OPE coefficients with their dependence on (f 0 ,f 0 ), the integration constants proportional to the black hole mass and charge respectively. We conjecture that in general, the lowest-twist OPE coefficients should be c ∆=n 1 d+2n 2 (d−1),J=2n 1 +2n 2 ∝ f n 1 0f n 2 0 . This generalizes to the results of [24] where only the n 2 = 0 case was considered.
• In section 4, we discuss the subtlety for integer ∆ L . In this case there will be logarithmic terms appearing in the solutions of the bulk linearized equation associated with the light operator. We formulate the construction for dealing with the logarithmic terms and give a few examples. The logarithmic terms log(zz) can be naturally interpreted as anomalous dimensions. We find that although the OPE coefficients mixed with double-trace operators cannot be fully determined, the anomalous-dimension related coefficients γ ∆,J can be. We exhibit and prove a formula of determining γ ∆,J in terms of the residue of OPE coefficients for non-integer ∆ L .
• In section 5, we turn to consider gauged supergravities and the supergravity inspired models where there are additional scalar fields involved in the black hole backgrounds.
We study two cases: (1) the light operator is outside the supergravity, (2) the light operator is part of the supergravity theory. For both cases, we find that in D = 5 gauged supergravity, even though c 4,0 = 0, there is no inconsistency because the additional scalars involved in the black hole have conformal dimensions ∆ = 2 and they can contribute to c 4,0 . Furthermore, we find that for the case (1), although the spectrum has ∆ = d − 2 operators, c d−2,0 is nevertheless vanishing. This issue can be resolved, however, by considering case (2) where the light operator is within the supergravity theory. For those light operators lying in the supergravity, ∆ L is, inevitably, an integer, for which we exhibit explicit examples for γ ∆,J and verify the equation found in section 4 again.
• In section 6, inspired by the study of supergravity cases in section 5, we turn to consider the general scalar hairy black holes. We show that we can always have c d,0 = 0 by considering scalar hairy black holes which contain either the operators with ∆ = d or the operators with ∆ = d/2.
• In section 7, we summarize the paper and present the outlook for future investigations.
• In Appendix A, the preliminary knowledge of conformal blocks is sketched.
• In Appendix B, the linearized equation for scalars in the variables considered in this paper is presented.

OPE coefficients from holography
In this section, we study the formalism using holographic technique to compute the heavylight four-point functions in the heavy limit. The formalism was developed in [24] for the case involving two light scalar operators and two heavy operators that are dual to the AdS planar black holes constructed in the pure gravity sector. We begin with the review of the formalism and then examine the consistency of the vanishing c d,0 for general even d.

Four-point functions and conformal blocks
We consider heavy-light four-point functions that contain two heavy operators O H with parametrically large conformal dimensions ∆ H ∼ C T , where C T is the overall coefficient associated with the two-point function of the stress tensor T µν . Two light operators O L have much smaller conformal dimensions, namely ∆ L ≪ C T . The four-point functions can be decomposed into conformal blocks G. In appendix A, we give a short review on conformal blocks and their properties associated with scalar four-point functions. In s-channel in the conformal frame, defined by (A.3), the four-point function can be decomposed as where ∆ HL = ∆ H − ∆ L , z andz are related to cross-ratios and c ∆,J 's are the products of two OPE coefficients, now commonly referred to simply as OPE coefficients. Note that c ∆,J 's also depend on ∆ L and ∆ H .
In the holographic picture, the state excited by a heavy operator in the heavy limit can be viewed as some asymptotically AdS spacetime while a light operator is some perturbation in this background.
In other words, the problem reduces to compute the linear perturbation of the corresponding dual bulk field in the black hole background and derive the two-point function using the standard holographic dictionary.
It turns out that it is advantageous to compute the four-point function in t-channel instead, namely which should be the same as the s-channel result because of crossing symmetry [16]. The four-point function in the light-cone limit z → 1 acquires a simplification since the heavy exchanged operators in OPEs in the t-channel would not survive. It follows that the exchanged operatorsÕ in t-channel are necessarily light operators with ∆ ∼ ∆ L in the spectrum.
When there is no confusion, for convenience, we simply drop off the tilde of the OPE coefficientc in (2.3) and replace z by 1 − z such that the light-cone limit becomes z → 0, i.e.
The fact that only G 0,0 ∆,J appears in the decomposition is sufficient to indicate that it is the t-channel four-point function. (For more relevant properties of conformal blocks G 0,0 ∆,J (z,z), see Appendix A.) Thus the holographic technique now amounts to calculating the two-point functions in the black hole backgrounds, comparing with the definition of the conformal blocks (2.4), and reading off the OPE coefficients.
This was carried in [24] for a free massive scalar in AdS planar black holes constructed in the pure gravity sector for even d dimensions. It was found that the lowest-twist OPE coefficients, i.e. c ∆,J with the minimum twist τ = ∆−J, are somehow universal in the sense that they do not depend on the details of the gravity theory under consideration. Since many of the results will be useful for the rest of the paper, we shall give a detail review of the construction in subsection 2.2 and 2.3.
The reason that one can treat the static |BH as the dual to a (heavy) scalar operator that appears in the four-point function (A.1) is that it is specified by the mass only with no spin. As we shall elaborate in subsection 2.4, there is a consistency check that the holographic OPE coefficient c d,0 must vanish for black holes in the pure gravity sector.
This was shown the case for d = 4 in [24]. We shall prove that c d,0 = 0 for general even dimensions in subsection 2.4, before we study more general matter supported black holes.

The construction in pure gravity backgrounds
As in [24], we consider here gravity minimally coupled to a free massive scalar where L(R µνρσ ) represents the generic higher-order curvature polynomials, and ℓ 0 is the bare AdS radius. For appropriate L, the theory admits an AdS vacuum of certain radius ℓ.
In the Euclidean signature and in planar coordinates, it is given by Here for simplicity, we set the AdS radius to unit. The boundary metric is assumed to be spherically symmetric. It is useful to introduce complex light cone coordinates (z,z): These are precisely related to the cross ratios in the conformal frame (A.3) discussed in Appendix A.
For the black holes in massless gravities, the parameter f 0 is related to the black hole mass. In the boundary CFT, f 0 has a universal interpretation in the sense that it only depends on the ratio ∆ H /C T , namely [24,45,46] The equation of motion for the free scalar φ around the black hole is given by where we assume that ∆ L ≥ ∆ L − d so that (∆ L − d, ∆ L ) are the conformal dimensions associated with the source and response modes respectively. The minimum conformal dimension is thus ∆ L = 1 2 d, corresponding to saturating the Breitenlohner-Freedman (BF) mass bound m 2 BF for the scalar φ. According to the standard AdS/CFT dictionary, the solution of (2.11) in the background (2.8) gives rise to the bulk-to-boundary propagator Φ(r, t, u) in which the coefficient of 1/r ∆ L is the two-point function. The coordinates (t, u) is related to (z,z) in the conformal frame (A.3) by (2.7). As we can see in Appendix A, the expression for conformal blocks can be complicated and few can be expressed analytically in closed forms. For general situations, one typically considers the OPE limit, namely taking z ∼z → 0. In this limit, the conformal blocks can be given order by order, e.g. (A.10) for G 00 ∆,J . The same situation arises for the bulk perturbation and one can solve the linear equation in the OPE limit. To do so, Ref. [24] made a change of coordinates In this coordinate system, the solution to (2.11) in the AdS vacuum (2.6) can be expressed simply as Thus in the pure AdS background, the light scalar propagator is simply (zz) −∆ L . Comparing to (2.4), it is natural to factorize the bulk-to-boundary propagator in general asymptotic AdS backgrounds as Φ(r, w,û) = Φ AdS G(r, w,û) . (2.14) Then the function G(r, w,û) in the r → ∞ limit is precisely the conformal block. In other words, the holographic dictionary now reduces to [24] O c ∆,J G 0,0 ∆,J (z,z) = lim r→∞ G(r, w,û) . (2.15) Note that the right-hand side of the above is convergent and therefore the subleading terms The near boundary expansion for G(r, w,û) therefore should take the form G(r, w,û) = 1 + G T (r, w,û) + G L (r, w,û) , where 1 represents the identity block 1 . Note that both w andû depend on r, it follows that G (T,L) (r, w,û) are both non-vanishing in the r → ∞ limit. When ∆ L is not an integer, the two sets are independent. As in [24], we shall focus on the the case of non-integer ∆ L . We shall comment on the case of integer ∆ L later.
As mentioned above, G T i (w,û)'s directly relate to conformal blocks with ∆ = (1 + i)d and G L i (w,û) relate to those with ∆ = 2∆ L + i = 2∆ L + 2n + J. Since the conformal block coefficients are non-zero only for even spin J, it follows that i for G T i must be even numbers. Since G T i and G L i should be related to the conformal blocks with certain ∆, they must take the polynomials ofû, The truncation to the finite orders of the polynomials ofû in (2.18) is subtle. To see this, one notices that the relevant term giving conformal block with ∆ is w ∆−mûm . If there were no such truncations, we would have However, as can be seen from (A.12), the lowest power for z in conformal blocks should be In fact, as we explain in Appendix B, the equation for G T contain a source supplemented by the background metric whilst the G L function remains source free and hence cannot be determine. The absence of any source is related to the fact that φ does not involve in the construction the background metric and hence there is no falloffs of the type 1/r ∆ L in the metric.
Consequently, the construction based solely on the asymptotic structure can only reveal the holographic OPE coefficients for multi-stress tensor contributions of heavy-light fourpoint functions in the heavy limit, while the double-trace contributions are far from clear.
For this reason, in this paper we in general simply drop the G L terms altogether (when it is source free), except in a few special cases where G L terms cannot be avoided.
It turns out that in even d dimensions, a ij (w) can be polynomials of w [24] a ij (w) = where the lower bound of the polynomial truncation for w is the same but in opposite sign to the upper bound of the truncation forû. This is because we simply let ∆−m → m in (2.19), and then we have m ≥ ∆ − J ≥ −J. Throughout this paper, we shall consider only even d dimensions such that we have the manageable polynomial ansatz (2.20). Consequently the exchanged multi-stress tensor operators all have even ∆ = nd conformal dimensions.
In fact, the solution a ijk contain poles ∆ L −n where n belongs to some finite set of nature numbers. Thus when ∆ L is itself an integer, the stress-tensor part of the contributions diverges. The requirement that the full solution be analytic in ∆ L indicate that b ij should also contain the same poles and all poles shall cancel each other such that the full solution is smooth. We leave further discussions on this issue in section 4.

Lowest-twist OPE from pure gravities
The important conclusion in [24] is that for the pure gravity AdS black holes, it turns out that the lowest-twist OPE coefficients of multi-stress tensor operators are universal with only the dependence of f 0 . For a given set of product operators of conformal dimensions ∆, the lowest-twist operator has the maximum possible J such that the twist τ = ∆ − J is minimum. For the multi-stress tensors T n we consider, the conformal dimension is ∆ = nd and the maximum spin is J = 2n. Thus the lowest twist operator is To isolate the lowest-twist contributions, we recall the analysis right below (2.19). The highest power ofû is the highest spin J for each conformal dimension ∆; therefore, it is advantageous to introduce ξ byû = r d/2 ξ. In the large r limit, then only the lowesttwist contributions become relevant at the leading order while all other contributions are suppressed. In other words, the ansatz of G in this limit becomes 22) and the scalar equation (B.2) is reduced to be It is now straightforward to see that only f 0 of the bulk background enters the equation.
The lowest-twist OPE coefficient depends only on f 0 , which is universally proportional to the ratio ∆ H /C T of the CFT parameters, as in (2.10). The ansatz for Q(w, ξ), following the analysis below (2.20), is given by Substituting it into (2.23) yields a recursion relation for a nm The OPE coefficients are related to a nm via As an example, we consider one stress-tensor n = 1. Its (maximal) spin is J = 2 and the lowest-twist OPE coefficient is [24].
We now would like to comment on the fact that the coefficients b ij cannot be determined by the equations of motion. This is not surprising since we are only looking at the solutions at the asymptotic expansion, without submitting them to the regularity constraints in the middle of the spacetime. What is highly non-trivial in the above approach is that the coefficients a ij can be nevertheless fully determined and hence all the OPE coefficients associated with the exchange of multi-stress tensor operators can be fully derived in even d dimensions. This is the consequence of the coordinate choice (w,û) and the solution ansatz proposed by [24]. As we can see in Appendix B, although the equation for G is homogeneous without a source, the effect of the ansatz is that the equation for G T has a source depending on the metric functions while G L remains source free.

Consistency of c d,0 = 0
The OPE coefficient c d,0 describes the exchange of a spin-0 operator of conformal dimension d. For pure (massless) gravity AdS black holes, together with a free scalar of non-integer ∆ L , the only candidate is the trace of the energy-momentum tensor. Thus we must have c d,0 = 0. This was shown for d = 4 in [24]. In this subsection, we examine the consistency for general even d.
First we examine the d = 4 case in some detail. For AdS planar black holes constructed by pure massless gravities, we must take f 0 = h 0 . We can nevertheless pretend that they are different for generality, in which case, we have On the other hand, the only possible operator contributing to c 4,0 in this setup is the trace of stress tensor T µ µ which must vanish due to the conformal symmetry. Thus the condition f 0 = h 0 which is always true for black holes constructed in pure massless gravities preserves the consistency T µ µ = 0. This demonstrates that in d = 4 AdS black holes constructed in the purely gravity sector is indeed dual to a scalar heavy operator in the heavy limit. The conclusion above is in fact true for all even d ≥ 4. To show this, we note that for n = 1, with maximum J = 2, G(r, w,û) involves at most quadraticû, namely Substituting (2.29) into equation (B.2), the constant coefficients a n and b n can be solved exactly in arbitrary even d dimensions. Theû 2 -order gives For even d, the series terminates at k = d/2 and hence we have where (i) j is the Pochhammer polynomial Theû 0 -order terms give rise to the recursion relation for a n : We thus end up with With the solution (2.34) and (2.31), both OPE coefficients c d,2 and c d,0 can be read off.
The c d,2 result in (2.27) can be reproduced precisely. We find that the coefficient c d,0 is (2.35) It is then clear that whenever f 0 = h 0 , we have c d,0 = 0, which signals the consistency for the construction. For a black hole constructed by pure gravity with only the massless graviton mode, we must have f 0 = h 0 . Furthermore, there is no more operator in addition to T µ µ that has (∆, J) = (d, 0). Thus c d,0 = 0 faithfully reflects that T µ µ is vanishing for CFTs in flat spacetime. On the other hand, for black holes involving additional matter, it is not uncommon that h 0 = f 0 , in which case c d,0 becomes non-vanishing. It is of interest to examine that the corresponding exchange operator indeed has (∆, J) = (d, 0).

The construction and explicit examples
In this section, we consider a general class of AdS black holes that are charged under a Maxwell field. We consider a general class of theories of the following form where L(R µνρσ , F µν ) represents the higher-order invariant polynomials of the curvature tensor and the strength F µν and hence matter and gravity can be generally non-minimally coupled. Higher-order gravity theories with higher-order Maxwell fields were studied exten-sively in the holographic context, see, e.g. [47,48]. As in the previous case, the black hole background associated with |BH does not involve φ, the free scalar that is dual to the light operator O L . As in section 2.2, the (massless) gravitational sector gives rise to the leading falloff 1/r d and its integer powers in the metric functions f and h due to the dimension analysis. Now by including the Maxwell fields, the black hole has additional falloffs 1/r 2(d− 1) and its integer powers in f and h. Furthermore, the dimension analysis implies additional terms 1/r nd+2m(d−1) with positive integers (n, m) are allowed. Thus charged AdS planar black holes have the following asymptotic expansion structure wheref 0 is proportional to Q 2 (the charge squared) of black holes. However, there is not yet any CFT interpretation analogous to (2.10) forf 0 , and it is not supposed to be viewed as a universal CFT parameter. Note in our notation, we would like to denote all the new terms created by the existence of Maxwell fields with positive sign, e.g. +f 0 . In general, when the linear spectrum of the AdS background contains only the graviton and massless vector modes, we must have h 0 = f 0 andh 0 =f 0 . For now, we leave them different so that the results are applicable in the more general situation.
The scalar φ equation in the black hole background has the same form (2.11), but now due to additional power appearing in (3.2), the ansatz for G(w,û) (2.17) should involve new power terms of 1/r. To be precise, we now have the power series where we simply drop the scalar double-trace mode contribution and denote the contributions from stress-tensor and conserved current as the "short" set G s (with identity block G 00 = 1). The additional power laws with 1/r 2(d−1) in (3.

3) indicate that by including
Maxwell fields, the conserved current operator J with conformal dimension ∆ = d − 1 and spin J = 1 should also appear to exchange in the scattering process and thus be involved in conformal blocks. However, J can only appear in pairs due to the even spin requirement for the conformal blocks, it follows that the minimum ∆ for the OPE coefficients that involve the Maxwell field is 2(d − 1), which is again an even integer. Following the same procedure outlined in section 2, we find that the OPE coefficients can be derived. We now present some explicit low-lying examples in d = 4 and d = 6 for general non-integer ∆ L .

d = 4
In d = 4, the near-boundary asymptotic expansions up to 1/r 10 for h and f take the forms The structures dictates the ansatz for G(r, w,û): 2) will yield the solutions for all (α 10 ij , α 01 ij , α 20 ij , α 11 ij ). The results are too large to present here and we shall give only the OPE coefficients here. The simplest case is ∆ = 4 and we have This is exactly the same as obtained in section 2. Thus for ∆ = 4, including the Maxwell field in the bulk solution gives no contribution to the OPE coefficients for ∆ = 4, and c 4,0 = 0 since we have f 0 = h 0 . This should be expected since the minimum ∆ for the Maxwell field in the conformal block is 6.
We obtain explicit OPE coefficients and the corresponding exchanged operators ∆ = 6, 8, 10: While the detail can be complicated, the structures of non-vanishing OPE coefficients and the relevant exchange operators can be derived from the dimension analysis. Up to and including ∆ = 10, each c ∆,J corresponds to one unique operator, the product of either T µν or J µ . For ∆ ≥ 12, c ∆,J can have contributions from multiple operators, via the product of both T µν and J µ . For example, to c 12,0 , both tr(T 4 ) and J 2 J 2 can contribute. As was in the previous cases, the OPE coefficients here also involve integer poles of ∆ L . We shall comment this in section 4. Note that the lowest twisted OPE coefficients such as c 4n,2n that exist in the previous section remains the same, depending only on f 0 , which have a universal CFT interpretation (2.10). The new lowest-twisted OPE coefficients such as c 6,2 and c 10,4 depend also only and simply onf 0 , analogous to the dependence of c 4n,2n on f 0 ; however,f 0 , being proportional to Q 2 , does not have a clear CFT interpretation. This is one of the rather common features in the AdS/CFT correspondence where a simple bulk quantity does not lands itself as a straightforward parameter in the dual CFT.

d = 6
In d = 6, we shall present the lowest-twist results up to and including ∆ = 16. This requires that metric functions (h, f ) expand to the order of 1/r 16 : The OPE coefficients for the lowest-twisted operators of the type c 6n,2n is the same as those in section 2 and they are universally depending on f 0 , unaffected by the Maxwell fields. However, including the Maxwell field in the construction of the bulk black hole does introduce new types of lowest-twisted operators. Here we present two explicit examples: .
These lowest-twist OPE coefficients depend only onf 0 and f 0 . In the next subsection, we show in general even d dimensions that the lowest-twist OPE coefficients with at most two current operators J µ depend only on the mass parameter f 0 and the charge parameterf 0 .

Lowest-twist analysis
We follow the analogous discussion in section 2. To isolate the lowest-twist contributions, we again take the largeû limit while keeping ξ =û/r d/2 finite and non-vanishing. As seen in section 2, we hope this allows us to select all the lowest-twist contributions for the pure multi-stress tensor parts T n in arbitrary even d. Here, we consider conformal blocks with n T µν 's and m J µ J ν 's, the lowest-twist contribution in G(r, w,û) has the large-r dependence (3.12) The contributions with higher twists forñ T andm J J fall as If we keep all orders up to O( 1 r m(d−2) ), then the condition that only the lowest twist contributions are preserved is (3.14) However, this condition cannot always be held. For example, for m = 2, we can easily find situations that violates the condition (3.14), e.g.m = 0, k = 1, d = 4. Thus we are not likely to isolate the lowest twist contributions. However, for m = 0 and m = 1, we find that (3.14) is always satisfied. In other words, we can take largeû limit and keep up to O( 1 r m(d−2) ) to isolate the lowest twist contributions with at most two current operators J µ J ν involved. Thus we shall consider two corresponding types of lowest-twist coefficients c ∆=nd,J=2n , and c ∆=(n−1)d+2(d−1),J=2n .
It should be emphasized that this restriction arises only because we would like to give the result for general d.
There is no such restriction if we consider a specific d.
In order to obtain the lowest-twist OPE coefficients with at most two current operators, we make the ansatz for G as Here Q (1) corresponds to c nd,2n and Q (2) corresponds to c (n−1)d+2(d−1),2n . Substituting Thus the general solution depends both f 0 andf 0 .

n = 1
The simplest case is n = 1, corresponding to J = 2. There are two lowest-twist OPE coefficients c d,2 and c 2(d−1),2 . We make the ansatz The solution for Q 2 , corresponding to c d,2 was obtained in [24], and presented in section 2, depends only on f 0 . The quantity Q 2 , corresponding to c 2(d−1),2 , satisfies the equation Subsequently, we have It follows from the analogous analysis below (2.20), we see that the lower cutoff must be −2 and that the upper cutoff must be 2(d − 2), i.e.
We now have a recursion relation for q m This can be solved straightforwardly, giving We find that the OPE coefficient c 2(d−1),2 is The d = 4 (c 6,2 ) and d = 6 (c 10,2 ) cases were already given in (3.7) and (3.12) respectively.

Recursion relation for general n
To obtain the OPE coefficients for higher conformal dimensions with at most two current operators, we take the ansatz (only for even d) The upper bound in the polynomial truncation for w is the conformal dimension. The recursion relation for all a nm was obtained in the previous section, see (2.25). Substituting .
The lowest OPE coefficients can be determined by a nm and b nm via c ∆=nd,J=2n = 1 2 J a n, d−2 To conclude this section, we would like to remark that in order to obtain a general formula for all even d dimensions, we restrict ourselves here to consider only the cases involving at most two current operators. We also worked out a few examples in some specific low-lying dimensions. Our results demonstrates that the OPE coefficients of the lowest-twisted operators involving n 1 stress tensor and 2n 2 current operators is proportional to f n 1 0f n 2 0 with purely numerical coefficients, namely

Anomalous conformal dimensions
For integer ∆ L , the short set G s alone diverges, we therefore have to take the double-trace set into account to fix the divergence. In general, the double-trace set, as ∆ L approaching a certain integer n, the (w/r) 2∆ L factor of G L (r, w,û) in (2.17) will have an extra logarithmic term, namely w r such that the factor (∆ L − n) in front of log w r will cancel the pole 1/(∆ L − n) in G L i and leave us a finite logarithmic term in the near-boundary expansion for G. We thus take the ansatz G(r, w,û) = On the other hand, we find that the all the coefficients of log(zz) can be fully determined by the equations of motion. To understand the the physical meaning of these logarithmic terms, it is worth noting that when ∆ L is an integer, taking r → ∞, the log r terms are not suppressed, and their coefficients are actually the conformal anomalies. For the convergent finite terms in the large-r expansion, in addition to polynomials of z andz that appear in conformal blocks, there are now terms with overall log(zz) and they do not appear in conformal block. We take the view that these log(zz) terms should be interpreted as anomalous dimensions for the exchanged operators of bare conformal dimension ∆. 2 Recall the conformal blocks G 00 ∆,J in the OPE limit [24], for small anomalous dimension ǫ, we have G 00 ∆+ǫ,J = G 00 ∆,J 1 + 1 2 ǫ log(zz) + O((ǫ log zz) 2 ) . As we shall see from an explicit example in the next subsection, the coefficients γ ∆,J can be completely determined from the asymptotic structure whilst the coefficients c ∆,J are not without imposing the boundary condition in the middle of the spacetime.

An alternative derivation
It is actually straightforward to understand why γ ∆,J 's could all be determined, since they can be derived directly from the c ∆,J 's discussed earlier. Recall that for the short set alone, the OPE coefficients have poles for integers ∆ L = n behaving like where A(∆ L ) is a regular function of ∆ L without poles. When ∆ L is an integer, c L ∆,J for the light exchange operators must mix with c s ∆,J with some specific (∆, J). As we have seen in the previous subsection, we may adopt (4.2) to obtain OPE coefficients c ∆,J which can be decomposed into c s ∆,J + c L ∆,J . The full OPE coefficients c ∆,J should be smooth for integer ∆ L = n. We can simply write c L ∆,J in terms the regular function c ∆,J as where U | ∆ L →n → 1. It follows from (2.17) that for ∆ L = n we have a prefactor in front of double-trace modes hence for double-trace operators we must have following terms Now we can conclude the coefficients γ ∆,J 's can also be readily read off as For those c s ∆,J without the pole ∆ L = n, even though some c L ∆,J will still mix with it, there will be no poles involved, then the factor (∆ L − n) in γ ∆,J simply suppresses it gives rise to γ ∆,J = 0. Therefore the formula (4.20) is still valid.
In the previous section we adopted the dictionary (4.5) to derive the low-lying γ ∆,J for d = 4 and ∆ L = 2 and d = 6, ∆ L = 6. It is easy to verify that these results can also be simply obtained from the explicit c ∆,J of general ∆ L in section 3. Thus many properties of c ∆,J 's will be inherited by the corresponding γ ∆,J . In particular, the γ ∆,J coefficient of the lowest-twisted operators involving n 1 stress tensor and 2n 2 current operators is proportional to f n 1 In this section, we consider AdS black holes in gauged supergravities where additional matter fields are involved. In particular, we consider charged AdS black holes in STU models which can be embedded in M-theory or type IIB strings as rotating branes via Kaluza-Klein sphere reductions [49].
The STU model was originally [50]  truncation, which sometimes is referred to as the D = 5 STU model. We follow the notation of [49] and write the Lagrangian for the bosonic sector as L = √ −gL, where The Lagrangian admits charged AdS planar black hole [49,51]. In the Euclidean signature, the solution is given by where we set the AdS radius ℓ to unity. To proceed on computing the holographic OPE coefficients, we first express the solution (5.2) in the form of (2.8). There is no close such a form, we present the metric in the large-r expansion. Define for large r, we have where we denote . To see this, we note that asymptotically, both (ϕ 1 , ϕ 2 ) vanish and their scalar potential, up to and including the quadratic order, is In other words, the scalars have the mass and dual conformal dimensions Therefore, the spectrum contains two different scalar operators with the same conformal dimension ∆ = 2, saturating the BF bound. They can contribute to the OPE coefficient Although everything discussed above appears to be consistent, the picture remains somewhat unsatisfactory. The first is that the free scalar is not part of the STU model, but introduced by hand. The second is related to the observation that there is no single scalar OPE coefficient, i.e. c 2,0 which could be contributed by either O 1 or O 2 . The vanishing of c 2,0 here is not itself inconsistent with the conformal blocks, but highly coincidental. In fact, both issues can be resolved within the STU model itself.

U(1) 2 truncation and perturbation
In the previous subsection, we introduced a free scalar propagating on the charged black hole in the STU model. The free scalar however lies outside of the STU model. In this subsection, we consider the scalar perturbation within the STU model, to examine whether the non-vanishing c 2,0 can emerge. The general perturbation is very complicated and we consider a special case. We truncate the U (1) 3 system to a U (1) 2 system by setting two out of three Maxwell fields equal, namely A 1 = A 2 ≡ A/ √ 2, in which case ϕ 2 = 0 decouples from the charged black hole. The metric of the resulting black hole can be simply obtained by setting q 2 = q 1 in (5.2), which means we have H 1 = H 2 . The large-r expansion has the same form, but the specific coefficients in each falloffs are specialized to q 2 = q 1 .
Instead of introducing a free scalar outside the theory, we start with the above reduced background with ϕ 2 = 0 and consider the linear perturbation We find that the linearized equation is + 4e where the quantities in the bracket are the solutions of the reduced U (1) 2 theory. Compared to the free scalar equation (2.11) where the mass is a constant, the "mass" in (5.9) is now r-dependent, and we may write (5.9) as The leading term of the large-r expansion of m(r) 2 is the constant mass squared which gives rise to the conformal dimension ∆ L . The first few terms for the expansion of m(r) 2 are The leading term tells us that ∆ L = 2 and it is an integer. Thus in this case, as was discussed in section 4, most of OPE coefficients are undetermined using the holographic procedure.
We can however derive the anomalous dimension related coefficients γ ∆,J , following the exact procedure outlined in section 4. We find some low-lying examples: It should be noted that the large-r expansion of m(r) 2 contains the 1/r 2 term, implying that the ansatz for G must also include the quadratic power 1/r 2 , which gives rise to nonvanishing c 2,0 . To obtain c 2,0 and also verify (5.13) using the general formula (4.20), we turn to consider (5.11) with a general ∆ L . The large-r expansion for f and h is assumed to take the same form as in (3.4). Following the same procedure, we find , . (5.14) Note that the OPE coefficients c 2,0 and c 4,2 remains convergent when ∆ L = 2. The other OPE coefficients become undetermined, as was discussed in section 4. It can be easily verified that the γ coefficients (5.13) can indeed be obtained from (5.14) using the formula (4.20). The non-vanishing of c 2,0 gives a more consistent picture that there is an exchange operator of ∆ = 2 in the spectrum. However, the procedure has the shortcoming in dealing with gauged supergravity models since the scalar fields are typically conformally massless with integer ∆ L .

D = 7 STU model
Seven-dimensional gauged supergravity from the Kaluza-Klein S 4 reduction of D = 11 supergravity have a consistent U (1) 2 truncation, the relevant bosonic Lagrangian is The charged AdS planar black hole was given in [49]. In Euclidean signature, it is The large-r expansion for f and h up to 1/r 10 in the metric coordinate choice (2.8) is Note in this case we have f 0 = h 0 andf 0 =h 0 . There is no new power lower than 1/r 6 ; however, a new term of 1/r 8 now appears in h. This term is contributed by the two scalars and reflects the non-vanishing results of c 8,0 . Indeed, from the potential in (5.15), it is easy to see that , . (5.22) When ∆ L = 4, as in the supergravity case, c 4,0 , c 6,0 and c 6,2 remains finite, but others become divergent and undetermined. Using the procedure outlined in section 4, we find that all the γ ∆,J coefficients however are fully determined, with the non-vanishing ones given by.
These coefficients can also be obtained by using the relation (4.20). The Lagrangian is

Supergravity inspired models
In this subsection, we only focus on the case with r dependent mass m(r) 2 . As in the previous STU models, we can consistently truncate ϕ 2 = 0 by requiring The resulting theory admits the the black holes in (5.25) with q 1 = q 2 . We then turn on the linear perturbation (5.8) and obtain the linearized scalar equation ( Thus we conclude that we have ∆ L = d − 2, and the lowest conformal block has conformal dimensions ∆ = d − 2.
We now turn to compute c d−2,0 with a general ∆ L . Since now the spin is zero, we are allowed to take the simplest ansatz for G as The equation (5.29) admits following exact solution . In this section, we study c d,0 in the context of general classes of AdS scalar hairy black holes. Recently large classes of exact hair black holes were constructed, see, e.g. [53][54][55][56][57][58]. Exact time-dependent solutions describing the formation of black holes were also constructed [59][60][61][62][63]. In this paper, however, an exact solution is not required in our analysis.
It is clear that the OPE coefficient c d,0 can be contributed by a single operator O of ∆ = d or by the product O 1 O 2 with ∆ 1,2 = d/2. In the latter case, we then should expect that a new coefficient c d/2,0 emerges in general. We shall discuss in detail how these issues arise and could be resolved in scalar hairy black holes.

AdS scalar hairy black holes and their asymptotic structures
For simplicity, we consider only one scalar Φ that is involved in the construction of the static AdS planar black holes. The relevant part of the Lagrangian in where the ellipses denote additional matter or curvature terms that can be involved in the solution but that do not affect our leading or sub-leading falloffs of the static black hole metric (2.8). Furthermore, the ellipses also include a new scalar φ whose linearized equation of motion in the black hole background takes the general form (5.10).
We first study the property of the scalar Φ. Assuming that V (Φ) has a fixed point Φ = 0 and the theory admits the AdS vacuum of radius ℓ = 1. For small Φ, we expect that V (φ) has the Taylor expansion We now consider AdS planar black holes involving Φ. The large-r expansions of (h, f ) and Φ can then be determined [64,65]. The leading and sub-leading terms are where Φ 1 and Φ 2 are constants. The Φ 2 2 terms above are determined by dimensional analysis; therefore, the dimensionless coefficients (c 1 , c 2 ) remains to be determined by a specific theory. The Φ 2 1 term in h is fully determined, by the equation This equation is generally true provided that Φ is the only scalar mode involved in the black hole.
At the first sight, the asymptotic structure appears to suggest that there are four in- It's back reaction to the metric functions are of higher orders such that h ∼ 1 − h 0 /r d + · · · and f ∼ 1 − f 0 /r d + · · · . Thus for minimally coupled scalar φ with (5.10), where m(r) is a constant, a non-vanishing c d,0 would naturally arise without introducing any issues.
We may also consider the possibility that the light operator φ couples to Φ, in the following way This types of coupling is inspired by the STU models discussed earlier. If the function u(Φ) for small Φ expands as then at large-r expansion, the m(r) 2 in (5.10) behaves as Now in addition to f 0 = h 0 , c d,0 also depends on α 1 Φ 1 . However, since Φ is not conformally massless, it does not typically arise in gauged supergravities.

∆ = d/2
When ∆ = d/2, the mass of Φ saturates the BF bound and the scalar is conformally massless in only d = 4. The large-r expansion for Φ is We require that Φ 1 = 0 for the AdS black hole. In this case, we no longer have f 0 = h 0 , but instead we have f 0 − h 0 ∼ Φ 2 2 . Now for d ≥ 6, the holographic OPE coefficient c d,0 depends not only on f 0 , but also on the Φ 2 2 . Introducing Φ with ∆ = d/2 to the black hole would imply the possibility of a new OPE coefficient c d/2,0 . This coefficient will be zero holographically if we consider the minimally coupled scalar φ. In order to generate a non-vanishing c d/2,0 , it is necessary to consider the coupling between Φ and φ, e.g.
where u(Φ) takes the same form as (6.7). Then we have m(r) 2 ∼ m 2 0 + α 1 Φ 2 /r d/2 + · · · in the large-r expansion. It would be instructive to present c d/2,0 explicitly. Assuming the metric does not have power 1/r d/2 , the equation can be solved for even d/2 and we end up For instance, for d = 4, (6.11) immediately gives rise to c 2,0 in (5.14) for the D = 5 STU model.

Conclusions
In this paper, we studied the holographic OPE coefficients for heavy-light scalar four-point proportional to f 0 − h 0 which is always zero in pure gravity black hole involving only the massless graviton. This is consistent with the fact that T µ µ = 0 for CFTs in flat spacetime. We then studied black holes involving matter fields that admit the possibility for f 0 = h 0 and hence necessarily exhibit more operators in the spectrum of the dual CFTs.
We included the Maxwell field and considered charged AdS black holes in a general class of gravity-Maxwell theories. The Maxwell field can contribute the conserved current operator J with ∆ = d−1, J = 1 to exchange in the conformal blocks in the boundary CFT.
The explicit low-lying OPE coefficients in d = 4 and d = 6 were presented. The recursion formula for the lowest-twist OPE coefficients involving at most two current operators were obtained. Our investigation indicates that the lowest-twist OPE coefficients associated with the charged black hole takes the form c ∆=n 1 d+2n 2 (d−1),J=2n 1 +2n 2 ∝ f n 1 0f n 2 0 where f 0 andf 0 are related to the black hole mass and charge respectively. However, the conserved current operator J is not lying in the track of c d,0 , which is consistent with the fact that charged black holes remain f 0 = h 0 .
Motivated by the fact that scalars in supergravities are typically conformally massless with ∆ L = d − 2, we studied the OPE coefficients when ∆ L is an integer. In this case, the solutions of the linearized scalar equation of the light operator involve logarithmic dependence and we presented a detail procedure to read off the coefficients γ ∆,J . Even though the OPE coefficients c ∆,J can not be fully determined, the coefficients γ ∆,J that are related to the anomalous dimensions can nevertheless be. In addition, we presented a general residue formula for extracting γ ∆,J from c ∆,J with generic ∆ L . For the charged black holes in gravity-Maxwell theories discussed in section 3, we find that for the lowest-twist operators we have γ ∆=n 1 d+2n 2 (d−1),J=2n 1 +2n 2 ∝ f n 1 0f n 2 0 . We then investigated the charged AdS black holes in D = 5, 7 gauged supergravity STU models and their generalization in general dimensions. These black holes not only involve multiple Maxwell fields, but also a set of scalar fields. As was mentioned earlier, the scalars are conformally massless and are dual to operators with ∆ = d − 2. In addition to following the earlier example and introducing a free scalar as the light operator, we consider linear perturbation of one of the scalars in the STU supergravity models. This allows to discuss the holographic properties within the context of supergravities. We obtained the OPE coefficient c d−2,0 explicitly. In D = 5, d = 4, although f 0 = h 0 and c d,0 = 0 owing to the scalar contribution, the results are consistent, since in d = 4, conformally massless scalars have ∆ L = 2, and hence a product of two of such scalar operators can contribute c d,0 . For ∆ L = d − 2, the coefficients γ ∆,J were also presented and verify the formula (4.20).
We analyzed the generic scalar falloffs in asymptotic AdS geometry. We found that c d,0 = 0 is not rare in the framework of scalar hairy black holes when the scalars that are dual to operators with ∆ = d or ∆ = d/2 are involved in the black hole construction.
Our preliminary investigation of the gauged STU models in section 5 indicates that the general procedure of the holographic OPE coefficients of heavy-light four-point functions can be analysed within the framework of supergravities. The price however is that ∆ L is now an integer such that the OPE coefficients are not fully determined. It should be emphasized that massive scalar modes also arise in supergravities in the Kaluza-Klein spherical reductions, but again they generally have integer ∆ L . For example, it follows from the general scalar formula in appendix A of [69] that the (massive) breathing modes in sphere reductions of M-theory or type IIB string give rise to massive scalars with ∆ L = 12, 10,8,6 in d = 6, 5, 4, 3 respectively. Scalars with non-integer ∆ L are hard to come by if not entirely impossible in the consistent truncation of gauged supergravities involving massive modes.
Thus the interior boundary conditions in all these cases must be required to constrain the linearized solution. However, the framework adopted in this paper is based on the nearboundary expansion. It is thus of great interest to develop new techniques to relate the interior data to the asymptotic values.

Acknolwedgement
We are grateful to Kuo-Wei Huang for clarifying for us the key points in their paper [24] at the early stage of this work. We are grateful to Jun-Bao Wu for useful discussion. We are also grateful to the JHEP referee for pointing out a serious technique error regarding to

A Conformal blocks
Conformal blocks capture the essence of the four-point functions in conformal field theories.
In this appendix, we present some properties of conformal blocks of scalar four-point functions. By the virtual of the conformal symmetry, the four-point functions can be written in a compact form To study the four-point functions, it is standard and convenient to use the conformal symmetry to take the conformal frame, namely x 1 = (0, 0, · · · ) , x 2 = (x, y, 0, · · · ) , x 3 = (1, 0, · · · ) , x 4 → ∞ . where λ ij∆ 's are the coefficients in OPE expansions and hence the three-point functions Throughout this paper, we actually denote c ∆,J = λ J 12∆ λ J 34∆ and call it an OPE coefficient. It should be thus understood that c ∆,J is not only a function of (∆, J), but also ∆ 12 and ∆ 34 . where (denoting a = − 1 2 ∆ 12 , b = 1 2 ∆ 34 ) where for (2.11) we have m 2 = ∆ L (∆ L − d), while for (5.10) m 2 is a function of r and the explicit form depends on theory detail. Changing the variables to (2.12) and factorizing the AdS propagator as in (2.14), we can present the equation for G explicitly as follows     The second equation contains a source that determines G T .
The situation becomes more complicated when ∆ L is an integer. The analysis of the scalar equation in this case is given in section 4.