The large D black hole dynamics in AdS/dS backgrounds

We have constructed a class of perturbative dynamical black hole solutions in presence of cosmological constant. We have done our calculation in large number of dimensions. The inverse power of dimension has been used as the perturbation parameter and our calculation is valid upto the first subleading order. The solutions are in one to one correspondence with a dynamical membrane and a velocity field embedded in the asymptotic geometry. Our method is manifestly covariant with respect to the asymptotic geometry. One single calculation and the same universal result works for both dS and AdS geometry or in case of AdS for both global AdS and Poincare patch. We have checked our final answer with various known exact solutions and the known spectrum of Quasi Normal modes in AdS/dS.


Introduction
Recently it has been shown ( [1]) that at infinite dimension limit, a finite number of quasinormal modes around any black hole solution are effectively confined in the near horizon region and are decoupled from the rest of the infinite tower of QNMs that extend upto asymptotic infinity. The spectrum also develops an infinite gap. In such cases it is natural that the decouple modes will have a closed dynamics among themselves even at nonlinear levels. The non-linear dynamics of these decoupled QNMs can be constructed in a power series expansion around infinite dimension (i.e., a series in 1 D ). This gives an algorithm to construct a new class of approximate solutions to Einstein equations with a dynamical event horizon. It turns out that there is a one-to-one correspondence between these nonlinear gravity solutions and a codimension one membrane, embedded in the asymptotic flat space, and whose dynamics is governed by a very particular equation, also determined in a power series in 1 D [2][3][4], see also [5]. See papers [6][7][8][9][10][11][12] for initial development of the subject of gravity at large D and inverse dimensional expansion.
In all the above cases, since the dynamics is confined in the near horizon region, it does not care much about the asymptotic geometry. This, in effect, implies that this whole 'large D' technique of solving gravity equations could be easily extended to situation where the asymptotic geometry is not exactly flat. We expect that the membrane-gravity correspondence will still hold for such cases, but now the membrane will be embedded in whatever non-flat asymptotic geometry (which we shall refer to here as 'background') we are interested in. In particular, similar construction should be possible in presence of cosmological constant, [16]. In [3] and [4], though the analysis is strictly applicable to asymptotically flat space, the final answer has been presented in this 'background-covariant' form. In [4], such covariance has been implemented even in the complicated intermediate steps for the derivation of the final metric upto the second subleading order.
In this paper, we have extended the formalism of [2,3], in a way so that this covariant dependence on the 'background' is manifest in every step. In addition we have also included cosmological constant, which could have any sign.
One of the key motivation to include the cosmological constant is the following. We know that in presence of negative cosmological constant, there exists another class of approximate solutions with dynamical event horizons which are dual to conformal fluids, living in a space with dimension one less than that of the bulk [27]. This duality holds in any dimension and therefore in large D as well. We would eventually like to see how the large D limit of these fluid modes map to the large D decoupled modes in presence of cosmological constant (see [16]). This paper is the first step towards this goal.
The organization of this paper is as follows. In section (2) we have described the initial set-up of the problem, the main equation that we would like to solve for and the scheme of our perturbation technique. In section (3) we described how in our scheme, different quantities scale with the dimension D, the perturbation parameter. In section (4) we have described how we could guess the leading ansatz. Next in a small section (5) we described how our approach becomes manifestly covariant with respect to the embedding geometry of the membrane. In section (6) we briefly explained the algorithm we used to solve for the first subleading correction. In section (7) and section (8) we have derived and presented the first subleading correction to the metric and the equation governing the dual membrane and the velocity field. Then in section (9) we have performed several checks on our ansatz. We have matched our solution with Schwarzschild AdS/dS black hole/brane and then with rotating black hole solution upto the required order in an expansion in 1 D . We have linearized our membrane equation and reproduced the known spectrum of quasi-normal modes . In an appropriate scaling limit of our equation (and after some linear field redefinition) we reproduced the effective hydrodynamic equation of [16]. Finally in section (10) we concluded. We have several appendices with the details of all computation.

Set-up
In this section we shall describe the basic set-up of our problem and the final goal in terms of equations. We shall also present the schematic form of the solution that we will eventually determine.
We are working with the following two derivative action of gravity.
where for Λ we have assumed the following scaling with dimension D. 1 .
Varying (2.1) with respect to the metric, we get the equation of motion.
As mentioned before, our goal is to find new 'black-hole type' solutions (i.e. metric with an event horizon) of equation (2.3) in a power series expansion around D → ∞.
Schematically the solution will have the form Here g AB is a smooth metric that also solves the same equation eq.(2.3). It is the metric that we have referred to as the 'background' in the previous section. On 1 See section (6) for the motivation of this choice 2 For our analysis in the later sections we shall often use a notation G AB 's together will capture the nonlinear dynamics of the 'decoupled quasi-normal modes'. Since the decoupled modes are confined within a thin region around the horizon, the G (k) AB 's should vanish fast as we go away from the horizon, implying that the g AB is the asymptotic form of the metric. As explained in [2][3][4], our final solution for G (k) AB 's will be parametrized by a codimensionone time-like membrane, embedded in the background space-time with metric g AB , with a velocity field along it. However the curvature of this membrane and the velocity field are not completely independent data. We can solve for G (k) AB 's consistently provided the extrinsic curvature of the membrane as embedded in g AB and the velocity field on it together satisfy some integrability condition which follows from the constraint equations of gravity. We would be viewing this integrability condition as a dynamical equation on the coupled system of the membrane and the velocity. This leads to a 'membrane-gravity' duality in the sense that for every solution of this membrane equation we shall be able to find a metric solution for equation (2.3) in an expansion in 1 D . Following [3,4] we shall determine G (k) AB 's in a way so that if we view the same membrane as a hypersurface embedded in the full space-time with metric G AB , it becomes the event horizon and the velocity field on it reduces to its null generators. components of the metric (modulo the coordinate redefinition freedom). So a naive large D limit, simply means that both the number of equations and the number of variables we would like to solve for, are blowing up along with our perturbation parameter.
To get rid of this complication, we shall implicitly assume that a large part of the geometry is fixed by some symmetry and the metric is dynamical only along some finite number of directions. In other words, the metric will be of the form [2] whereG ab ({x a }), {a, b} = {0, 1, · · · , p} is a dynamical finite (p + 1) dimensional metric and dΩ 2 is the line element on the infinite (D − p − 1) dimensional symmetric space. f ({x a }) is an arbitrary function of {x a } which is not constant.
Since the metric is dual to a membrane embedded in the background g AB with a velocity field along it, the symmetry of the metric must be there in the membrane, the velocity field and the background as well. This will imply that the dual membrane is dynamical only along the x a directions and simply wrap the symmetric space (with metric Ω AB ). Similarly the dual velocity field must have components only along the x a directions and also the nonzero components should not depend on the coordinates along the Ω-space. As a consequence, the same feature (i.e., no components along the symmetry directions and all nonzero components are functions of x a 's only) would be true of any vector constructed out of the membrane data. Similarly for tensor structures the components, where all indices are along the isometry directions, must be proportional to the metric in the symmetric space, Ω ab . In such cases we could easily see that for any generic vector or one form, the order of its divergence will always be D times larger than the order of the form itself [2][3][4]. In fact such a rule will apply to tensors with any number of indices. If T A 1 A 2 ···An is a generic tensor of order O 1 D k maintaining the symmetry of equation (3.1), then In the same way we could see that if the background metric g AB admits a decomposition of the form (3.1), then the Riemann tensor evaluated on g AB will be of order O(1) and Ricci tensor and Ricci scalar will be order O(D) and O(D 2 ) respectively.
It follows that the Einstein tensor evaluated on g AB would be of O(D 2 ) 3 and since we want g AB to satisfy equation (2.3), it justifies our choice of D scaling for the cosmological constant as given in equation (2.2). However as explained in [4], for our calculation we do not need any details of the decomposition as given in equation (3.1) or the symmetry itself. The only aspect of it that will be used is the scaling law (3.2) and the D dependence of the curvatures, evaluated on g AB .

Leading Ansatz
In our calculation G (0) AB is the starting ansatz that captures the nonlinear dynamics of the decoupled modes at the very leading order. Any perturbation theory works provided we have a clear guess for what should be the leading answer. In this sense, we can carry on with our program only if we know the appropriate form of G (0) AB that solves the equation (2.3) at leading order in 1 D expansion. So we shall first describe how we could guess the form of this leading ansatz.

The form of the leading ansatz
As mentioned before, the two parameters that will characterize our solution are a codimension-one hypersurface, embedded in the background space-time with metric g AB , and a unit normalized velocity field u µ defined along the membrane 4 .
We shall first construct a smooth function ψ of the background coordinates {X A } such that (ψ = 1) gives the equation for the membrane. Next we shall construct a smooth one-form field (O = O A dX A ), defined everywhere in the background spacetime, such that the projection of (−O A ) along the membrane reduces to the velocity vector field u µ . We shall determine our final solution in terms of this bulk function ψ and bulk one-form field O. Note, at this stage there is a huge ambiguity in the construction of ψ and O. The condition, they have to reduce to something specific on ψ = 1, is certainly not enough to fix them completely. We shall fix this ambiguity with certain convenient choice (see subsection (6.2) for a more detailed discussion on this point). At this stage the simplest structure that we could imagine for G (0) AB (that does not involve any derivative of the two basic fields ψ and O) is the following where F is any arbitrary scalar function of ψ and (O · O) 5 . From equation (4.1) it follows Here all raising/lowering and contractions are with respect to the background metric g AB . Now firstly we want ψ = 1 surface to be the horizon when embedded in the metric G AB . This implies that (∂ A ψ)(∂ B ψ)G AB = 0 on ψ = 1. Now we shall impose this 4 Throughout this paper, we shall use Greek indices to denote indices along the world volume of the membrane as embedded in g AB , whereas capital Latin indices will denote full space-time indices. The velocity field u µ is unit normalized with respect to the induced metric along the membrane (denoted as h µν ) .
u µ u ν h µν = −1 5 Throughout this paper '·' denotes contraction with respect to the metric g AB condition order by order in 1 D expansion. At leading order it implies Secondly we want the velocity vector field to be the null generator of the horizon, which is given by Also by definition, the projection of (−O A ) along the membrane will give the velocity field. This in turn implies In equation (4.4) to go from second to the third line we have used equation (4.3). From equation (4.4) it follows that On the other hand using the fact that velocity vector field on the membrane (viewed as a hypersurface embedded in the background g AB ) is normalized to minus one, we see From equations (4.5) and (4.6) it follows that at leading order in 1 D expansion, O is a null one-form with respect to the background metric g AB .
We shall often express O A as By construction u A is always along the membrane and it will be the velocity field u µ , if expressed in terms of the intrinsic coordinate of the membrane. So far from our analysis we could see that the simplest form of G (0) AB is the following.
is zero at leading order, F could only be a function of ψ, if we do not want any derivative at zeroth order. We also want F to be vanishing outside a thin region of thickness of order O 1 D around ψ = 1. This would be ensured provided F (ψ) ∝ ψ −D . Now in equation (4.3) if we substitute the fact O is null at leading order, we find This fixes the proportionality constant in F to be one. So finally we are lead to the following expression for our leading ansatz 6 It turns out that this form will solve equation (2.3) at leading order provided the following conditions are satisfied (see [2,3] for a more detailed discussion) As before, the membrane ψ = 1 is viewed as a hypersurface embedded in the background space-time with metric g AB and ∇ A denotes covariant derivative with respect to g AB .

When ansatz solves the leading equation
Now we shall demonstrate that given the D scaling law (3.2) and (3.3), how G AB as given in equation (4.10) indeed satisfies the equation (2.3) at leading order. We shall simply evaluate the gravity equations on the metric G (0) AB plus the background g AB and we shall see that leading order (which will turn out to be of order 6 We would like to emphasize that what we have presented here is not a derivation for the leading ansatz. In the end this is a 'guess' and our perturbation program is developed around this starting point. This guess could also be motivated from the fact that our final solution, in a very small patch of size of the order of O 1 D , looks like a D dimensional Schwarzschild black hole with a local radius and boost velocity. See [3], [4] for a more detailed discussion on this O(D 2 )) piece vanishes provided the conditions as mentioned in equation (4.10) are satisfied.
Before getting into any details, we shall first simplify the equation (2.3) a bit, by subtracting the trace part of the equation.
Now we shall evaluate R AB on the metric G AB . Details of the calculation are presented in appendix (B). Here we are simply quoting the final result.
where •R AB is the Ricci tensor evaluated on the background g AB • ∇ A denotes the covariant derivative with respect to background metric g AB • K is the extrinsic curvature of the membrane as embedded in the background: . Therefore the leading equation reduces to Since O A and n A are two independent vector directions in the background spacetime, equation (4.13) finally implies Equation (4.13) is simply the conditions mentioned in equation (4.10). Note also that at leading order the RHS of equation (2.3), which captures the effect of cosmological constant, does not contribute. Also note that the two equations in (4.13) together imply that Here u is defined in equation (4.8) 7 5 Covariance w.r.t. 'background' metric In this section we shall discuss how we could recast all subsequent calculation in a manifestly covariant form with respect to the background g AB . In fact this feature has already appeared in the previous section (see equation (4.12)). As we know, the computation of R AB , to begin with, involves partial derivatives of the metric components G AB . However, the expressions appearing in (4.12) have only covariant derivatives with respect to the background g AB . In [4] this point has been argued from a physical point of view and has been used extensively.
Here we shall see how it follows algebraically. This is a consequence of the fact that though Christoffel symbols are not covariant tensors, their differences are and therefore the Christoffel symbols on the full metric G AB could always be written as the Christoffel symbols evaluated on the background g AB plus a correction which will have a form of a covariant tensor with respect to the background. Then this feature could easily be extended to the construction of the Riemann tensor and the Ricci tensor for the full background.
The general form of our metric Let us denote the Christoffel symbols corresponding to G AB as Γ A BC , whereasΓ A BC denotes the Christoffel symbols corresponding to the background g AB .
where ∇ A denotes the covariant derivative with respect to g AB . In deriving equation (5.1) we have used the fact that Christoffel symbols are symmetric in its lower two indices. Now in our convention, Ricci Tensor, R AB , of the full metric is given by the following expression. Using equation (5.1) we could easily rewrite it in a covariant form.
whereR AB is the Ricci Tensor evaluated on the background and δΓ A BC is the covariant tensor appearing in the second term of equation (5.1) Equations(5.1) and (5.2) are the key equations that we shall use to determine the subleading corrections to the metric in a manifestly covariant fashion.
6 General strategy for the first subleading correction Once the leading ansatz G (0) AB , the function ψ and the one-form O are well-defined everywhere in the background with metric g AB , we can describe the strategy to determine the subleading corrections to the metric i.e., the G (k) AB s for k > 0. In this paper our goal is to determine G (1) AB . Our method is essentially same as the one described in [4]. The purpose of this section is to mainly set up the notation and convention. We shall omit any detailed justification or 'all order proof', for the statements. Interested reader should refer to [4] for a thorough discussion.

Summary of the algorithm
We already know that if we evaluate Ricci tensor on G  AB . Then at order O (D), the equation of motion (4.11) will have two pieces. One piece will take the form of a linear differential operator acting on different (and so far unknown) components G  AB . The first piece will have an universal structure at all orders and we shall call it as 'homogeneous piece' or H AB . The second part will be termed as 'source' (S AB ) . Schematically Our solution procedure will essentially be an 'inversion' of the universal differential operator in H AB .
We shall determine G (1) AB completely in terms of the function ψ and the one-form O, that are directly related to the basic data of our construction -the membrane and the velocity field. One advantage of our formalism is that we never need to choose any specific coordinate system on the membrane or for the background g AB .

Subsidiary condition
Note that so far all the conditions on ψ and O are imposed only along the membrane. We want ψ to be one on the membrane hypersurface and the projection of O onto the membrane to reduce to the velocity field u µ . The gravity equation (2.3) at leading order (see equation (4.14)) imposes some more constraints on ψ and O, but still they needed to be satisfied only at (ψ = 1). Therefore there is a large ambiguity in the construction of the function ψ and the one-form O. In this subsection we shall fix this ambiguity with a certain convenient choice, which, following [2], [3], [4], we shall refer to as 'subsidiary conditions'. 8 .
Subsidiary condition on ψ is chosen as follows.
It could be shown that equation (6.1) is enough to determine ψ in an expansion in 1 D around the membrane (ψ = 1) [28]. Also we could easily see that (6.1) is consistent with the second equation (4.14)(See appendix (E)). Now we shall describe how we fixed the ambiguity in the definition of O A . Unlike ψ, since O A is a vector in the background with D components, we need D equations to fix it completely. From the construction of G (0) AB we know that on the membrane, O A is a null vector and O · n = 1, where n A in the unit normal to the membrane. Firstly note that once we have imposed equation (6.1), (ψ = constant) surfaces and therefore the unit normal to them are well-defined everywhere. Therefore we could easily lift these two conditions on O, which are initially imposed only on the membrane, to everywhere in the background. In terms of equation what we mean is the following O · O = 0 and O · n = 1 everywhere (6.2) Equation (6.2) gives two scalar conditions on O. We still need (D − 2) equations through which we would be able to determine the remaining (D − 2) components O A , everywhere in the background . To fix them we use the following differential equation.
Since P A B is the projector to the subspace orthogonal to both n and O, equation (6.3) is effectively a collection of (D − 2) equations as required 9 . Equations (6.2) and (6.3) together fix the ambiguities in all components O, everywhere in the background.
It is possible to rewrite the subsidiary condition on O in a more geometric form. Equation (6.2) and (6.3) it follows that Equation (6.4) simply implies that throughout the background geometry, O A s are the tangent vectors to the null geodesics passing through the membrane.
In course of analysis we shall often define a u A field everywhere in the background 10 .
Note that as a consequence of equation (6.2), u A turns out to be a unit normalized time-like vector, which is orthogonal to n A by construction.
Also the projector P AB of equation (6.3) is actually a projector orthogonal to both n A and u A and therefore could equivalently be expressed as

Choice of gauge
We shall choose a gauge such that 10 Equation (6.5) apparently looks very similar to equation (4.8). However the main difference is that equation (6.5) is true for any constant ψ slices whereas equation (4.8) was specifically applied to the membrane i.e., (ψ = 1).
Note that our leading ansatz also satisfies this same gauge.
After imposing equation (6.6) the most general structure for G (1) AB is the following Here the unknown scalar, vector and the tensors, Note the extra factor of 1 D in the term proportional to P AB . This is because, by definition, G AB is the collection of those terms in the metric that contribute to the gravity equation at order O(D). As we shall see below, the term proportional to P AB will contribute one extra factor of D in some terms of the gravity equation (the ones that involve a trace of the metric tensor). In other words, unless we suppress this term by an extra factor of 1 D , it will contribute and mess-up the matching and solving of the equations at order O(D 2 ).

The form of explicit ψ dependence
We know that within the region where the metric correction is nontrivial, (ψ −1) is of order O 1 D . Therefore we would define a new order O(1) variable R ≡ D(ψ − 1) to parametrize the explicit ψ dependence of the unknown scalar, vector and the tensor functions in equation (6.7). In terms of equation we mean the following.
Here f n (R), v n (R), t n (R) and h n (R) are functions that do not involve any explicit factors of D. The other expressions, s n , [v n ] A , [t n ] AB are the different scalar, vector and the tensor structures of order O(1), involving the derivatives of n A and O A that could appear at order O(1). The upper limit for the sum over n will generically be different in scalar, vector and tensor sector. These structures, by construction will not have any explicit dependence on ψ, since all such explicit dependence at this order will be captured by the function f n , v n , t n and h n . However these structures will depend on ψ implicitly through the derivatives of n A and O A . But note that this will be a 'slow' dependence in 1 D expansion. More precisely if we compute of the variations of s n , v n or t n in the direction of ∂ A ψ it will always be of O(1), whereas the variations of f n (R), h n (R), v n (R) and t n (R), will be of order O(D). This is the reason, we could treat these structures, s n , [v n ] A and [t n ] AB effectively as constants when we are doing the leading order computation with G (1) AB . See the next subsection for details.

Structure of 'Homogeneous piece'
In this subsection we shall list the detailed form of the homogeneous piece. As mentioned before, the homogeneous piece could be computed by simply linearizing the gravity equations (4.11) around as G Here X ′ for any function X(R) denotes dX dR .
From the explicit expressions of H AB it follows that where Π AB is the projector perpendicular to (ψ = 1) hypersurface as embedded in the background.
It turns out that we could easily decouple these homogeneous parts of the E AB by taking the following linear combination of the components.

Structure of 'Source'
In general the source S AB will depend on all the coordinates, through some explicit dependence on ψ and also through different derivatives of O A and n A . As before, we can classify the ψ dependence of S AB as 'slow' and 'fast'. The 'fast' pieces are those whose derivatives in the directions of increasing will have a factor of D, (i.e., the dependence on ψ is through R ≡ D(ψ − 1)). These are the parts which have been treated exactly at a given order. All other variations of the source terms, both along and away from the membrane hypersurface, are 'slow' (i.e., the derivatives are suppressed by a factor of 1 D compared to the 'fast' dependence) and therefore could effectively be treated as constants while solving for the next correction to the metric i.e, G AB . This is why we simply invert the homogeneous piece H AB assuming it to be an ordinary differential operator in the 'fast' variable R. See [2] and [3] for a more detailed explanation.
As we have seen in the previous subsection, the projected components of the ho- could be viewed as ordinary second order differential operator in the 'fast' variable R, acting on the unknown functions appearing in the metric correction. It follows that to determine the unknown functions f (R), v(R) and t(R), it is enough to solve the projected components the gravity equations (4.11) or The traceless piece of the projected E AB leads to the following set of second order inhomogeneous differential equations for three sets of the unknown functions, f n (R), v n (R) and t n (R).
In equation (6.19) we have also used the fact that Note that the last two equations in (6.19) will admit regular solutions at ψ = 1 only if We shall see that both of these conditions will be true as a consequence of our membrane equation. In fact in [2] this is the regularity condition that has been used to determine the membrane equation.

Boundary condition
Since our differential operator (in R) is second order, we need two sets of boundary conditions to fix the integration constants. One of these is the 'normalizability' . In our construction it must be true that the metric is non-trivial only in a thin region of thickness O 1 D around the membrane ψ = 1. This defines the normalizability conditions on the metric functions f n (R), v n (R), t n (R) and h n (R); in R coordinates they must vanish exponentially as R → ∞ (recall R = ψ−1 D ), so that outside the 'membrane region' the metric is that of the background. This 'normalizability' fixes one integration constant in each of the three differential equations in (6.19). It turns out that for equation (6.20) both the zero modes are non-normalizable or in other words in this case the 'normalizability' condition is enough to fix h n (R).
The other integration constant is fixed by the condition on the horizon. For f n and v n it is fixed by our definition of the horizon itself. We want ψ = 1 to be the exact equation for the horizon of this geometry and u A to be the null generator of the horizon. This implies that the following 'all order' equation on the horizon Note that by construction at any order the metric will take the form Now (6.22) fixes the values of f and V A on ψ = 1 or equivalently R = 0.
For the tensor sector i.e., the function t n (R), the other integration constant could be fixed by demanding the solution is regular at the horizon.

Solution in the form of integral
Once the boundary conditions are fixed, we can explicitly invert the differential operators and could write the solutions for f n (R), v n (R), t n (R), and h n (R) in terms of some definite integrals of the source. In this subsection we shall present these formulas explicitly.
As mentioned before in subsection (6.6) we could always rewrite source S AB at any given order as some functions of 'fast' variable R multiplied by the 'slowly' varying scalar, vector or tensor structures relevant for that order. In other words the RHS of the three equations in (6.19) could be expressed as Similarly RHS of (6.20) could be written as Now we can explicitly write the solution for G (1) AB in terms of definite integral of the source.

G
(1) Here K s and K v are two constants added so that

Constraint and membrane equation
Consider the following combinations of different components of H AB .
Note that the above combinations have at most one R derivative of the unknown functions. Clearly the same feature would be true if we take the above combinations on the components of E AB , since the source S AB does not involve any of the unknown functions. Hence these combinations could be viewed as equations that restrict the 'initial conditions' (defined on any constant R slice) for the second order differential equations (see (6.19)) controlling the 'R-evolution' of the unknown functions. It follows that the 'constraint' equations in our case has the following form In terms of source S AB and the unknown metric functions, the above two constraints will take the following structure 11 Now it is known that if the constraint is satisfied along one slice and the dynamical equations are satisfied everywhere, then the constraint is automatically satisfied along all hypersurfaces [29]. In [4], this theorem has been explicitly verified for the constraint equations listed above in equations (6.30). Because of this theorem, we are allowed to impose the constraints (6.30) only on ψ = 1 hypersurface and do not 11 We know that given the foliation of the space-time with ψ = const hypersurfaces, the equations of gravity could be decomposed into dynamical and constraint equations [29]. The constraint equations are the ones where one of the indices of the Einstein equation is projected along the normal to the foliating hypersurfaces. In [4], this theory has been used and explained in detail the context of our large D expansion. Along with the two combinations we mentioned in equations (6.29) one more constraint equation appears in [4], whose abstract form is the following However, we shall not analyze this combination here since it will not be required to obtain the final gravity solution and the membrane equations worry about how these equations are solved away from the membrane. So at order O(D), the final form of the membrane equations In deriving equation (6.31) we have used the fact that O A = n A − u A and v n (R = 0) = 0 because of our boundary condition. We also used the fact that T AB is regular at R = 0 due to choice of integration limits (see equation (6.27)) and thus the term involving unknown tensor metric correction in C A vanishes at R = 0. Equations (6.31) are the genuine membrane equations that do not involve any of the unknown functions and therefore only constrain our membrane data. Also note that these are the combinations that appear in the RHS of the first two equations in (6.19) and the regularity of the solutions also demand the vanishing of these constraints on R = 0.
The fact that given a solution to these constraint equations along the membrane, we can always solve the other dynamical equations (i.e. the other components of the E AB ), by inverting the linear differential operator appearing in H AB , establishes the 'membrane-gravity duality' that we have mentioned in the introduction. 7 The first subleading correction: G In this section we shall describe how we calculate the first subleading correction to the metric along with the coupled equations of motion for the membrane and the velocity field along it. As described in the previous section, at this order the source S AB will be simply be determined by evaluating the Ricci Tensor R AB on the metric G The details of the computation of the Ricci Tensor are presented in the appendix (B). Here we simply take the appropriate combinations of the different components equation of motion. For convenience we quote the final answer for the source at first subleading order.

Constraint equation
In the previous section we have described how we could determine the constraint equations on the membrane by taking appropriate combination of the components of the source terms evaluated at ψ = 1. In this subsection, we shall first evaluate those combinations on S AB and determine the constraints on the membrane data at the first subleading order. Note that at leading order there was only one scalar constraint on the membrane data It turns out that at first subleading order we shall have one scalar and one vector equation. This matches with the number of free data we have on the membrane: the shape of the membrane (scalar function) and the unit normalized velocity field on it (the vector function).

Constraint in the vector sector
First we shall describe the constraint equation in the direction perpendicular to u A .
We shall refer to this as 'Vector constraint'.
In the last step we have used the subsidiary condition (6.3). Now we shall substitute the following identity in place of P C B ∇ 2 O C as derived in appendix(E) Note that once we substitute equation (7.3) in equation (7.2), all derivatives and the all the indices (both contracted and free) are projected along the hypersurface (ψ = 1). Now it is easy to rewrite the constraint equation as an equation intrinsic to the membrane.
Here∇ denotes the covariant derivative with respect to the intrinsic metric of the membrane. K µν is the extrinsic curvature of the membrane, viewed as a tensor intrinsic to the hypersurface and K is the trace of K µν .

Constraint in the scalar sector
Now we shall describe the constraint equation in the scalar sector, i.e.,the constraint in the direction of u A .
In the last line we have used the following identities (see appendix (E) for proof).
As before, this equation also could be written purely in terms of the intrinsic data of the membrane. Note that where∇ denotes the covariant derivative with respect to the intrinsic metric of the hypersurface (ψ = 1) viewed as a membrane embedded in the background. Combining equations (7.5) and (7.7) we finally find

Dynamical equation
In this section we shall give details of the dynamical equations. It turns out that given our subsidiary condition and after imposing the scalar and vector constraint equations, the sources for all dynamical equation simply vanish leading to the vanishing of G AB .

Tensor sector
From the first equation of (6.19) we get the relevant differential equation for the 'tensor-type' correction at the first subleading order.
But from equation (7.1) we could simply see that In the language of equation(6.25) it implies that S tensor n (R) vanishes for all (n). Substituting this in the first equation of (6.27) we find T (1) AB is zero.

Vector sector
From the second equation of (6.19) we get the relevant differential equation for the 'vector-type' correction at the first subleading order.
Note that the RHS of equation (7.10) implicitly depends on ψ. However the dependence is 'slow', in the sense as one goes away from (ψ = 1) hypersurface, the variation of the RHS is suppressed by a factor of 1 D . Thus, at this order, we need to evaluate the RHS only at (ψ = 1) hypersurface. Now from equations (7.2) and (7.4) it follows that In the language of equation(6.25) it implies that S vector n (R) vanishes for all (n). Substituting this in the second equation of (6.27) we find V (1) A is zero.

Scalar sector
In the scalar sector there are two unknown functions h(R) and f (R) and therefore we need two equations. Clearly equation (6.20) and the last equation of (6.19) are the relevant equations here.
Now since P AB S AB vanishes, the boundary conditions (see section (6.7) ensure that h n (R) is zero for every n. Given that h n (R) is zero and there is no correction in the vector sector (implying v (1) n (R) is zero for every n) the second equation of (7.11) reduces to Now, following the same logic as we have used in 'Vector sector' , the RHS of equation (7.12) is simply the scalar constraint equation and therefore vanishes. Now the boundary conditions ensures that f n (R) = 0 for every n.

Final metric and membrane equation
In this section we shall simply summarize our final result i.e., the metric and the membrane equation of motion upto the first subleading order. As we have seen in the previous section, given our subsidiary condition, the next to leading correction to the metric vanishes.
where the scalar function ψ and O A are defined everywhere in the background (with metric g AB ) through the following equations Clearly the asymptotic form of the full space-time is given by the metric g AB , which we have referred to as 'background'. ∇ is the covariant derivative with respect to g AB . The equations (8.2) are enough to fix ψ and O everywhere provided the shape of the (ψ = 1) hypersurface and the one form field O A on (ψ = 1) hypersurface are given.
We have referred to these two pieces of information as 'membrane data' . It turns out that (8.1) is a solution of the gravity equation provided the membrane data satisfy the following equation of motion is an equation intrinsic to the membrane, in the sense that all raising and lowering of indices and the covariant derivatives are defined with respect to the induced metric on the membrane -a hypersurface embedded in the background g AB . All the indices now can take (D − 1) values. K µν is the extrinsic curvature tensor , viewed as a tensor structure defined on the membrane only. K is the trace of K µν . The velocity field u µ is the projection of the one form O A along the hypersurface. And P ν µ is the projector perpendicular to the velocity field u µ . Like the extrinsic curvature tensor, this projector is also defined only along the membrane worldvolume.

Checks
In this section we shall perform several checks on our solution for the metric and the equation of motion for the membrane.

Matching with known exact solution
We know of few exact static and stationary black hole / brane solutions of the equation (2.3) in arbitrary dimension. Now our effective membrane equation (8.3) and the metric (8.1) are valid as long as the number of dimensions is very large. Clearly static and stationary exact solutions are special cases which must solve our equation and must match with our metric in the appropriate limit. In this subsection we shall show this matching explicitly for three different exact solutions in Asymptotically AdS space.

Schwarzschild Black-Brane in AdS
In Kerr-Schild form AdS-black brane is given by where dS 2 Poincare is the line element in Poincare patch AdS space.
For the black-brane geometry (9.1), the hypersurface r = 1 is the horizon and the null generator of the horizon is given by It follows that the dual membrane is given by the same surface r = 1, however viewed as a hypersurface embedded in the AdS space with metric dS 2 Poincare and the velocity field along the horizon is simply u = −dt. The induced metric on the membrane We can easily see that this velocity field u is divergence free along the membrane. It is very easy to compute the extrinsic curvature tensor for this configuration. The non-zero components of extrinsic curvature and trace of extrinsic curvature are given by All the components of the derivatives of the velocity field on the membrane vanisheŝ Substituting equations (9.3) and (9.4) in the membrane equation (8.3) and using the fact that P t t = P t i = 0, we see that it is satisfied upto the required order. Next we shall match the form of the metric. For this we need to read off ψ and u A in such a way that 1. ψ = 1 surface is same as the r = 1 surface. In other words if we consider ψ as a function of r, then ψ(r = 1) = 1.

u
3. Both ψ and the u A satisfy the subsidiary conditions (6.1) and (6.4).
The normalized form of u is easy to guess.
Translation symmetry in t and all i directions guarantees that ψ must be a function of r alone and it follows that the subsidiary condition on u is trivially satisfied (since any vector in the space perpendicular to n ∼ dr and u ∼ dt must vanish because of the symmetry). Now we shall solve for ψ in an expansion in 1 D . Let us start by expanding ψ around the horizon r = 1.
Here a 10 , a 11 , a 20 are constants (to be determined by solving the subsidiary condition (6.1)) and we have also used the fact that within the 'membrane region' (r − 1) ∼ O 1 D . Substituting (9.6) in (6.1)) and solving order by order we find Note that equations (9.7) and (9.5) imply that in the 'membrane region'

Schwarzschild Black-Hole in Global AdS
In Kerr-Schild form of global AdS black holes are given as where dS 2 Global is given by Horizon of this black hole space time ((9.9)) is located at the zero of the function f (r) = 1 + r 2 − r −(D− 3) , The null generator of the horizon is given by It follows that our membrane is given by the hypersurface r = r 0 embedded in the AdS space with metric as given by dS 2 Global and the velocity field along the horizon is simply u = − 1 + r 2 0 dt. The induced metric on the membrane We can easily see that this velocity field u is divergence free along the membrane. It is very easy to compute the extrinsic curvature tensor for this configuration. The non-zero component of the extrinsic curvature and the trace of extrinsic curvature are given by Where Ω ab is the metric on (D − 2) dimensional unit sphere (9.11) All the components of the derivatives of the velocity field on the membrane vanisheŝ Substituting equations (9.3) and (9.4) in the membrane equation (8.3) and using the fact that P t t = P t a = 0, we see that it is satisfied upto the required order. Next we shall match the form of the metric. As in previous subsubsection we have to read off appropriate ψ and u A defined everywhere in Global AdS space.
• Since the space-time is static and also maintains spherical symmetry, ψ must be a function of r only. This implies n A dx A ∝ dr. After normalization n A dx A = dr √ 1+r 2 .
• It follows that the normalized u has the form It is easy to see that this u will satisfy all the subsidiary condition as a consequence of the symmetry.
• Now ψ has to satisfy the subsidiary condition, To solve the equation (9.14) we have to repeat the same procedure as we have done in the previous subsubsection. Now the only difference is that the background is not AdS-Poincare but global AdS and the covariant derivatives are also modified accordingly. This calculation is a bit complicated and the details are given in appendix (C) Here also (9.15) imply that in the 'membrane region'

Rotating Black Hole in AdS
The explicit form of Kerr de-Sitter metric in D = 2n + 1 dimensions( [30], [31]) in Kerr-Schild form is given by g µν is actually the metric of global AdS, but written in some rotating coordinate. The coordinate transformation that will bring it back to standard form (the one presented in equation (9.9)) is given in [30]. However we shall continue to work in the coordinates as given in equation (9.18). One of the advantage of using these coordinates is that the horizon of the black hole space time in these rotating coordinates is given by constant r slices, where the value of the constant is determined from the zero of the following function.
For convenience of computation we shall scale the parameter M in the following way so that the horizon lies at r = 1, which would be the equation of our membrane. The induced metric on the membrane It turns out that k µ is null with respect to both the metric g µν andḡ µν . The null generator of the horizon is given by From here it follows that the velocity field along the horizon is given by Once we have the explicit form of the membrane equation and the velocity field, each term of (6.31) are computable. Now as we have explained before, our 1 D expansion is valid provided the spacetime satisfies some large symmetry and is dynamical or non-trivial only in a finite number of dimensions. The metric in (9.17) will belong to this class, if only a finite number rotation parameters a i 's are non-zero. But if we turn on arbitrary (though finite) number of a i ' s, it turns out that explicit computation is very tedious for this complicated metric. So we have used Mathematica (version 9.0) here and to be explicit we have used two non-zero rotation parameters. We have first checked that this velocity field and the extrinsic curvature of the membrane do satisfy our membrane equation (8.3) upto the required order.
The next job is to check whether the space-time metric (9.17) matches with equation (8.1) upto correction of order O 1 D 2 . Now we know that k A is exactly null with respect toḡ AB . Clearly k A is the most natural candidate for the null vector O A we have in our metric. Suppose where A is some unknown function of r at the moment. Now note that the metric (9.17) will be precisely of the form (8.1) provided we identify The above equation along with the fact that A is a function of r , will imply that ψ also depends only on r. The unit normal to ψ = constant slices is then given by Now O A n A = 1 implies k A n A = A. Therefore once we know the explicit expression of n A , we can fix A. It turns out A = √ F

However just identifying A 2 2M
U with ψ −D is not enough for the matching of the two metrics. We also have to see whether these ψ and O A satisfy our subsidiary conditions. The above identification will be consistent with our subsidiary condition (6.1) provided Here ∇ is defined with respect to the background metricḡ AB and all raising and lowering of indices have been done usingḡ AB . In Mathematica we have explicitly verified this condition for two nonzero rotation parameters.

Quasinormal Modes for Schwarzschild black hole in background AdS/dS spacetime
In this subsection, using our membrane equations we shall compute the spectrum of light quasi normal modes for Schwarzschild Black hole with horizon topology S D−2 × R in background AdS/dS spacetimes. We will find that the QNM frequencies that we get match exactly with the earlier obtained result from purely gravitational analysis done in [32]. We do this calculation in Global AdS/dS coordinates. The background AdS/dS in global coordinates can be written as The black hole solution in this coordinate system has the following form In equation (9.28) r 0 is an arbitrary constant. From now on we choose r 0 = 1 for convenience. After we find the answers for QNM frequencies we can reinstate these factors easily from dimensional analysis. As we have seen in the previous subsection, a static black hole corresponds to a spherical membrane with a velocity field purely in the time direction. Here we introduce a small fluctuation around this spherical membrane along with a small fluctuation in the velocity field. The amplitude of the fluctuation will be denoted by ǫ -the linearization parameter for our analysis.
Here a indices denote the angle coordinates along the (D − 2) dimensional sphere and the coordinates along the membrane (i.e., time t and angles a) are denoted by µ indices. The induced metric on the membrane worldvolume upto linear order in ǫ is given by (with the components denoted by g Normalization of the velocity field (u µ g µν (ind) u ν = −1) implies The membrane equations have the following form Here∇ denotes the covariant derivative with respect to the metric (9.30). K µν is the extrinsic curvature viewed as a symmetric tensor along the membrane world volume. K is the trace of K µν and the projector (again as a tensor along the membrane world volume) perpendicular to u µ is denoted as Different components of this projector are given by Now, for convenience we rewrite the vector membrane equation (second equation in (9.84)) as Note that because of the spherical symmetry of the background E a (remember 'a' denotes the angle coordinates along the sphere) will be nonzero only if fluctuations are present or in other words E a ∼ O(ǫ). Also P t t = 0 and P a t ∼ O(ǫ). It follows that the time component E tot t identically vanishes at the linear order. Now since P t a = O(ǫ), we see that only O(ǫ 0 ) pieces of E t matter in the computation of E tot a . We keep these facts in mind and evaluate only those terms in E µ that will be important for our linearized analysis.
First note that K µν is generically not equal to the (µν) component of K AB , the extrinsic curvature viewed as a tensor in the full background space-time. K µν is given by the pullback of the extrinsic curvature on the membrane surface as where we have denoted the set (r, t, θ a ) by X M and the set (t, θ a ) by y µ . The spacetime form of extrinsic curvature K AB is given by Now if we apply equation (9.35) for our case, we find From explicit computation we know (see appendix D.1) that K rN = O(ǫ). It follows that for this linearized analysis K µν is just the 'truncation' of the K M N evaluated on the membrane surface and is given by (see appendix D.1 for details).
Here∇ a denotes the covariant derivative with respect to the metric on a (D − 2) dimensional unit sphere. The trace of the Extrinsic curvature is given by Thus the components that would be relevant for the linearized membrane equation are given by In writing (9.41) we have also neglected the terms which are subleading in 1/D. We also need to process the first equation of (9.84). We have to evaluate the divergence of the velocity field. It comes out to bê Now, similar to calculation done in Section (5) of [3] we divide the fluctuation δu a in two parts δu a = δv a +∇ a Φ , with∇ a δv a = 0 (9.43) Substituting (9.43) into (9.42) we get Now consider∇ a E tot a . Using the identity∇ a∇2 V a = ((D − 2) +∇ 2 )∇ a V a and simplifying we get Note that compared to the flat case (refer to Eq. (5.16) in [3]), it is easy to see that the only term extra in equation (9.45) is the last term which is crucial. We expand the fluctuation as where the scalar spherical harmonics Y lm on S D−2 obeȳ After substituting (9.46) in (9.45) and solving we get the scalar QNM frequencies Reinstating the factors of r 0 we get This exactly matches with the result given in [32] in Section 4. Now we find the vector QNM frequencies. Since we have solved (9.45) the δr and Φ terms in (9.41) drop out and the equation reduces tō We expand the fluctuation as where the vector spherical harmonics Y lm a on S D−2 obeȳ Substituting (9.51) in (9.50) and solving we get the vector QNM frequency as Reinstating the factors of r 0 we have This also exactly matches with the result given in [32] in Section 4.

Nonlinear effective equations for AdS Black brane dynamics from scaled membrane equations
In a parallel development, the authors of [16] have developed an effective theory for black brane dynamics in background AdS spacetime. They focus on the length scales of order 1 √ D and derive a pair of nonlinear effective differential equations that govern the dynamics of fluctuations which are suppressed for large D by appropriate inverse powers of D given in [16]. In this section we show that by doing appropriate scalings in our membrane equations, we are able to reduce our membrane equations to the form that matches the effective equations given in [16] under appropriate field redefinition. This analysis is very similar to the one done for the case of black pbrane in flat spacetime in [34]. In this section, we first do the linearized analysis of fluctuations without any scalings and get idea about how the various quantities need to be rescaled. Then we do the nonlinear analysis by applying the scalings and show the correspondence to effective equations of [16].

Linearized fluctuation analysis and hints for scalings
Now we do the linearized fluctuation analysis for AdS Schwarzschild black brane with horizon topology R D−2 × R in Poincare patch metric. We will consider fluctuations that depend only on p number of dimensions (with p ∼ O(1)), in the sense that the shape and velocity fluctuations will be function of some p coordinates. And also the velocity fluctuations will be only in the same p directions.
The background metric in Poincare patch (with AdS radius L = 1) is given by Where the indices a, b take p number of values. We will only consider fluctuations in these directions as mentioned above. The indices i, j take D − p − 2 number of values. Letr = r 0 be the position of static unperturbed black brane in Poincare patch coordinates. We choose to scale the coordinates with r 0 in the following waŷ In these scaled coordinates the background metric takes the following form And also the position of the membrane is now at r = 1.
When we introduce the fluctuations on this membrane we will consider the time dependence as e −iωt = e −iωt , withω = r 0 ω We work with this choice from now on. Note that with this choice all the new (non-hatted) coordinates are dimensionless. As mentioned before, in this section we shall consider small fluctuations around a static blackbrane solution. The fluctuations will be of the form ǫ is the linearization parameter.
To the leading order in ǫ, the induced metric on the membrane worldvolume is As before, we use the notation∇ for denoting the covariant derivative constructed from the induced metric (9.59) and ∇ for denoting the covariant derivative constructed from the background metric (9.57). In this notation the membrane equation will have the same form in as in equation (9.84), where P µν , K µν and K are the projector, extrinsic curvature and its trace exactly as in previous section. K µν is given by the pullback of the space-time extrinsic curvature K M N on the membrane. Here also using the same reasoning as in the previous subsection one could show that K µν is just the 'truncation' of the K M N evaluated on the membrane surface. The nonzero components of K µν are given by t δr − (1 + 2ǫδr), K ta = −ǫ∂ t ∂ a δr, K ab = −ǫ∂ a ∂ b δr + (1 + 2ǫδr)δ ab (9.60) Thus the trace of Extrinsic curvature becomes where the index a in (9.61) is raised with δ ab . Normalization of the velocity field fixes u 0 and δu t , defined in (9.58), in terms of the radial fluctuation u t = u 0 + ǫδu t = −(1 + ǫδr) (9.62) Given the velocity field, different components of the projectors P µ ν = δ µ ν + u µ u ν are given by Now, following the same trick as in the previous subsection we denote the vector membrane equation (the 1st line in (9.84)) as Then we have Note that both the background and the fluctuation preserve translational symmetry along the x i directions. Therefore i component of any vector must evaluates to zero on this perturbed background. Thus the i component E tot i identically vanishes at the linear order. On the other hand the background has a translational symmetry along the x a directions that is broken by the fluctuations. Hence E b ∼ O(ǫ). Now using the facts that P t t = 0, P a t ∼ O(ǫ) and E b ∼ O(ǫ) we can see that the time component E tot t vanishes at the linear order. For E tot a , since P t a ∼ O(ǫ), we see that only O(ǫ 0 ) pieces of E t contributes. We keep these facts in mind and calculate only those terms that are important.
and (with the notation ∂ 2 = ∂ a ∂ a ) u µ K µa = −ǫ∂ t ∂ a δr + ǫδu a , (u ·∇)u a = ǫ∂ t δu a + ǫ∂ a δr (9.66) Using equation (9.64) the expression for linearized E tot a is given by Note that if we assume all spatial and temporal frequencies are of order O(1), then in equation (9.67) the last two terms in parenthesis are suppressed compared to the first three terms by a factor of 1 D . However, it turns out, that the temporal and the spatial frequencies are related by a factor of 1 √ D even if we ignore the last two terms in equation (9.67), mentioned above. This happens because in the scalar sector the divergence of the velocity fluctuation couples to the shape fluctuation (i.e., δr) and the coupling is through equation (9.68) which involves a relative factor of D. This simply says that it is inconsistent to assume both the temporal and spatial frequencies to be of order O(1). Now we shall demand that the temporal frequency is of order O(1), but we shall not restrict the spatial frequencies. In that case the terms in the first parenthesis in equation (9.67) are certainly suppressed compared to the first three terms, but the terms in the last parenthesis need not be. Thus for our purpose E tot a is given by One might wonder that since we are considering the fluctuations with k ∼ O( √ D), there might be instances where the subleading correction terms in the membrane equations of motion will contribute at the same order as the terms present in (9.69) and (9.68). But one can carefully think that this will not happen. The only type of potentially dangerous terms are where we have (∇ 2 ) n (with n > 0) in the numerator. But since action of each∇ 2 raises the order of the term by D, there would be a corresponding factor of D n in the denominator, and thus the order of this term will be still subleading compared to terms present in (9.69) and (9.68), even if k ∼ O( √ D). Now we find the scalar and vector QNMs of the membrane. Finding ∂ a E tot a and substituting (9.68) we get We can compare (9.70) with the analogous equation that can be derived for black p-brane in flat space as was done in [34] and we note that the equation remains the same as in [34] except that now the first term has negative sign. As we will see this sign difference implies that there is no instability in shape fluctuations unlike in the case of black p-brane in flat space. Now we consider the plane wave expansion of the fluctuations as δr = δr 0 e −iωt e ikax a (9.71) Thus substituting (9.71) into (9.70) and solving we get the scalar QNM frequencies Thus the most general solution to (9.70) is given by δr = δr 0 1 e −iω 1 t e ikax a + δr 0 2 e −iω 2 t e ikax a (9.73) where, Now we can take the form of the most general solution of δu a which solves (9.68) and (9.69) as (Note there is only one vector QNM frequency as (9.69) has at max one time derivative acting on δu a ) where V 1 a and V 2 a are vectors in the direction of k a and v a is any vector such that v a k a = 0. Putting (9.75) into (9.68) and (9.69) we get Thus we see that there is no instability in AdS case. We write again the most general solution to the equations (9.69) and (9.68) where, From (9.77) and (9.78) we see that the interesting length scale along the x a directions is 1 √ D , rather than the scale of order unity we take. Next we work in the scaled limit adapted to capture the physics at length scale 1 √ D .

Scaled nonlinear analysis and derivation of effective equations
From the analysis in the previous subsection we could see that if we want the frequency along the time direction to be of order O(1), then the spatial frequency k has to be very high, of the order of O √ D . To zoom into this regime, in this subsection we work with the scaled spatial coordinates x a → y a = √ D x a . The spatial frequencies in the new coordinate will scale ask a = ka √ D . Therefore in the regime of interest the frequency along the new space coordinates will be of order onẽ k a ∼ O(1). AdS Poincare patch metric (9.57) takes the form Now suppose we repeat the linearized analysis of the previous subsection in these new coordinates. We shall normalize the fluctuations such that the components of the velocity vector field in the directions of ∂ y a are of order O(1). It follows that [u · dy a ] ∼ O 1 D . In old x a coordinate we already know the solution of [u · dx a ] (see equation (9.75) and the second equation of (9.77)). Solution in new coordinates will simply be the coordinate transform of the old solution. In other words if we expand the velocity field as With this coordinate redefinition the metric (9.79) becomes ( dy a dy a D +dx i dx i ) (9.81) In this scaled coordinate system the fluctuations are of the form where Y , u 1 and U a are all of order O(1) in terms of (1/D) expansion. Now we shall substitute these fluctuations in our 'membrane equation' and evaluate it at very leading order in (1/D) expansion. However now we shall not consider any linearization with respect to the amplitude of the fluctuations. The procedure for evaluating the equation of motion is very similar as in the previous two subsections. So we shall be very brief here. The metric induced on the membrane worldvolume is given by where z µ ≡ Coordinates along the membrane ≡ {t, y a , x i } (9.83) We use the notation∇ for covariant derivative with respect metric (9.83) and∇ for covariant derivative constructed from metric (9.81). In this notation the membrane equation is given by µν + u µ u ν (9.84) As before K µν is given by the pullback of the extrinsic curvature tensor K M N expressed as a tensor in the full background metric.
Here we have denoted the set (ρ, t, a, i) by X M and the set (t, a, i) by z µ . Now from explicit calculation we see that K ρN ∼ O(D −2 ) (see appendix D.2.2). Hence here also K µν is just the 'truncation' of the K M N evaluated on the membrane surface and the nonzero components are given by where the rest of the components are zero. Normalization fixes the time component of the velocity field in terms of its spacecomponent. 87) The answer for the membrane projector P µ ν = δ µ ν + u µ u ν is given by Now, we denote the vector membrane equation (the 1st line in (9.84)) as Note that E i and E tot i won't contribute in the leading order analysis as both the background and the fluctuations satisfy translational symmetry along x i directions. Also we know from explicit computation that the leading terms in E a are of order O 1 D . Thus it is easy to see that we only need to evaluate the quantities E t to order O(1).
At leading order it is easy to see that E tot t = −U a E tot a . Thus the only independent components of the membrane equation are along y a directions. The relevant terms are given by (keeping terms of leading order in 1/D) Thus we now can evaluate E tot a and is given by Also the equation∇.u evaluates to Equations (9.91) and (9.92) are the two effective equations for the membrane variables (membrane's shape and the velocity field on it) at leading order. Now we shall perform a variable redefinition which will recast these equation exactly as given in [16].
of the euqations (9.91) and (9.92) are just the effective equations derived in [16] which are (in the notations used in this paper) Thus we see from this procedure that the effective equations derived in [16] are just a particular scaling limit of our membrane equations. Note that our leading order membrane equations were derived in systematic expansion in 1/D. But in this section we have rescaled our membrane equation to consider the length scales of order 1 √ D . Strictly speaking, this is beyond the regime of validity of our membrane equations. But it can be argued that this scaling is a consistent thing to do, in particular, the most general terms that can be written as subleading corrections to our membrane equations do not get so much enhanced so as they become comparable to the leading order terms in the membrane equations. The argument goes just like given in the Discussion of [34] for black p-brane in flat spacetime and we won't rewrite here.

Conclusion and Future Directions
In this paper, we have used 'large D' techniques to find new dynamical 'black hole' solution to pure Einstein equations in presence of cosmological constant. The solutions are determined in an expansion in 1 D and are in 'one-to-one' correspondence with a dynamical membrane (characterized by its shape and a velocity field on it) embedded in the asymptotic geometry (which could be AdS or dS). The method we have used is manifestly covariant with respect to this asymptotic geometry (which we have referred to as 'background'). We do not need to choose any coordinate system for the background geometry at any point of our derivation. The same calculation works for both global AdS and Poincare patch. The form of the final answer also remains invariant. However, they are different solutions with different asymptotic geometries and horizon topologies and this fact is encoded in the various covariant derivatives that appear in the final solution. These covariant derivatives are always defined with respect to the background. We have applied this method to calculate the metric and the governing equation for the dual dynamical membrane upto the first subleading correction. Then we have performed several checks for our universal coordinate independent answer, by specializing to different coordinate systems.
• We matched them against the known exact and static solutions -Schwarzschild black hole/brane and Myers-Perry black holes for both asymptotically AdS and dS spaces.
• We have linearized our membrane equations and matched them against the known spectrum of black hole/brane QNMs in AdS space and black hole QNMs in dS space.
• We have taken a special scaling limit of our equations and recovered the dual effective hydrodynamic equations that was determined in [16] for the AdS blackbranes in large number of dimensions.
One immediate future direction would be to extend this calculation to the second subleading order. As described in [28], this is the order where we expect the leading entropy production for dynamical black holes. Also it would be easy (though tedious) to generalize this analysis to Einstein-Maxwell system in presence of cosmological constant. It would be interesting to calculate the stress tensor and the entropy current for this system following the method developed in [28]. For AdS space we know there exists another perturbative technique to construct new gravity solution that are dual to fluid dynamics in one lower dimension [27]. This duality works in any dimension [35] and therefore in particular large number dimensions where we can also apply 1 D expansion. It would be very interesting to explore how these two perturbative techniques could be patched together. AB . Let us denote the perturbed metric as Also, as it is clear from our discussion, in this linearized calculation we need to compute only the leading D piece. The linearized variation of the Christoffel symbols and the Ricci Tensor take the form AB . Now we can easily convert D A to ∇ A (i.e. the covariant derivative w.r.t g AB ) by introducing some new terms to account for the correction to Christoffel symbols generated from the extra piece

A.1 Scalar sector
In this subsection we shall compute H scalar AB . The relevant part of δG AB has the following form.
So finally

A.2 Vector sector
In this subsection we shall compute H vector AB . The relevant part of δG AB has the following form.
Now we shall substitute equation (A.8) in each of the four terms in equation (A.2).
So finally

A.3 Tensor sector
In this subsection we shall compute H tensor AB . The relevant part of δG AB has the following form.
Now we shall substitute equation (A.12) in each of the four terms in equation (A.2). (A.14)

A.4 Trace sector
In this subsection we shall compute H trace AB . The relevant part of δG AB has the following form. As explained in section (6), we have an extra factor of 1 D compared to the expressions of δG AB in tensor, vector and the scalar sector.
So finally Note that in the above equation, the second line is of order O(1). Since in our calculation we are only interested upto order O(D), we could ignore the second line.

For our purpose
B Calculation of the sources -S AB In this section we shall give details of calculation of S AB . As mentioned in subsection (6.6) we have to evaluate E AB on G [0] AB .
WhereR AB is the Ricci tensor evaluated on the background metric g AB and δR AB is simply the difference between the Ricci tensor evaluated on G [0] AB and Ricci tensor evaluated on g AB . Using this notation S AB = δR AB − Dλ G Now for our case, As the one form field 'O' is null, the inverse of the above metric (B.3) becomes very simple.
Substituting lead ansatz in equation (5.3) we find Here ∇ is covariant derivative with respect to the background metric g AB . For the convenience of computation we shall decompose δΓ A BC in two parts From (5.2) we know that Ricci tensor can be written as From equation (B.5) it follows The expression for δR AB simplifies once we substitute equation (B.5) In the last step we have used (6.4). Similarly, Term-2 = 0 (B.14) Now we shall compute Term-1, which is non-zero and a bit complicated.
Now using the fact that we finally find δR (2) AB | non-lin.
In the last line we have used the fact that Now we proceed to the calculation of δR We can use identity(E.1) to simplify (B.17) In the last step we have used the subsidiary condition on O A .
Finally, δR AB | non-lin. becomes Now we will calculate the linear terms in Ricci tensor In the last step we have used subsidiary condition on O and also the fact that Here we have used the fact that within the 'membrane region' ψ = 1 + O 1 D

C Intermediate steps for matching with AdS Black Hole
Since we know that the horizon is not at r = 1, this implies ψ(r = 1) = 1. We shall assume the following expansion of ψ around r = 1.
where X 1 , X 2 , a 10 , a 11 , a 20 are constants and (r − 1) Substituting equation (C.1) in equation (9.14) and solving it order by order in 1 D we find the following solutions for the coefficients. a 10 = 1, a 11 = X 1 − 2, a 20 = 0 (C.2) To fix X 1 and X 2 we have to use the fact that ψ = 1 correspond to horizon. We can determine the horizon of Schwarzschild-AdS black hole r 0 order by order in 1 D .

D.2.2 Scaled nonlinear analysis
The nonzero Christoffel symbols for the metric (9.81) are The normal to the membrane surface is given by (D. 16) The projector P M N = δ M N − n M n N is given by where the rest of the components are zero. The answer for∇ M n N is given bȳ ,∇ a n ρ = O(D −2 ),∇ ρ n a = O(D −2 ), where the rest of the components are zero.
The answer for spacetime form of the Extrinsic curvature K M N is where the rest of the components are zero. Nonzero Christoffel symbols components for the induced metric (9.83) are given by 20) The answer for∇ µ u ν is given bỹ where the rest of the components are zero.

E Identities
In this appendix we shall prove some identities that we have used for our computation.