Near Horizon Symmetry and Entropy Formula for Kerr-Newman (A)dS Black Holes

In this paper we provide the first non-trivial evidence for universality of the entropy formula $4\pi J_{0}^{+}J_{0}^{-}$ beyond pure Einstein gravity in 4-dimensions. We consider the Einstein-Maxwell theory in the presence of cosmological constant, then write near horizon metric of the Kerr-Newman (A)dS black hole in the Gaussian null coordinate system. We consider near horizon fall-off conditions for metric and $U(1)$ gauge field. We find asymptotic combined symmetry generator, consists of diffeomorphism and $U(1)$ gauge transformation, so that it preserves fall-off conditions. Consequently, we find supertranslation, supperrotation and multiple-charge modes and then we show that the entropy formula is held for the Kerr-Newman (A)dS black hole. Supperrotation modes suffer from a problem. By introducing new combined symmetry generator, we cure that problem.


I. INTRODUCTION
It seems that any valid theory of quantum gravity must incorporate the Bekenestein-Hawking definition of black hole entropy [1,2] into its conceptual framework. The black hole has a thermodynamical entropy as where S BH is the Bekenstein-Hawking entropy, A is the area of the event horizon and l P = ( G c 3 ) 1 2 is the Planck length. One may be ask, what is the microscopic origin of this entropy? Although the various counting methods have pointed to the expected semi-classical result, there is still a lack of recognition as to what degrees of freedom are truly being counted. Recently, motivated in great part by the recent works of Hawking, Perry and Strominger [3,4], it has appeared that a new way to approach the information paradox for black holes lies in a careful analysis of near horizon symmetries and the existence (in 4 dimensions) of an infinite-dimensional asymptotic symmetry group, the bms 4 group (For a good review and references, see [5]). Also, recently the authors of [6] have obtained a very simple horizon entropy formula, for black hole solutions in 3D Einstein gravity, where J ± 0 are zero mode charges of U (1) current algebra near horizon. In our previous paper [7] (see also [8]), we have studied the near horizon symmetry of spacelike warped AdS 3 black hole solutions of Generalized Minimal Massive Gravity (GMMG) [9]. Similar to the near horizon symmetry algebra of the black flower solutions in Generalized minimal massive gravity [10], the near horizon symmetry algebra of the warped black flower consists of two U (1) current algebras, with different levels. We have shown that the formula (2) exactly works for warped black flower solutions. So these investigations give us a non-trivial evidence for universality of this simple entropy formula in the context of 3D gravity. More recently an analog of the above entropy formula emerged in the near horizon description of non-extermal Kerr black holes in 4-dimensions [11], Now an interesting question is this :"if the simple entropy formula (3) is again as universal as its 3dimensional pendant (2)" [11]. Therefore, in order to investigate universality of the entropy formula (3) beyond pure Einstein gravity in 4-dimension, we consider the Einstein-Maxwell theory in the presence of cosmological constant. We show that this entropy formula give us the correct results for Kerr-Newman (A)dS black holes. We show that Kerr-Newman (A)dS black holes in 4-dimension Einstein-Maxwell exhibit an infinite-dimensional symmetry in their near horizon region.

II. CONSERVED CHARGES IN EINSTEIN-MAXWELL THEORY
First of all, we briefly review the approach of the covariant phase space method for obtaining conserved charges in Einstein-Maxwell Theory. To do this, we follow references [12][13][14][15][16]. Suppose spacetime (M, g) is globally hyperbolic and orientable. Suppose Φ is a collection of dynamical fields. The Lagrangian of Einstein-Maxwell theory is a functional of metric g µν and the gauge field A µ , then in this theory, we have Φ = {g µν , A µ }. The Lagrangian of given theory is written as where here R, F µν = ∂ µ A ν − ∂ ν A µ and Λ are respectively the Ricci scalar, electromagnetic field strength and the cosmological constant. First order variation of the Lagrangian (4) is in which E Φ have dual indices with Φ and sum on Φ is explicitly assumed. In the equation (6), Θ µ [Φ, δΦ] is the surface term and we refer to it as symplectic potential. Also, E Φ = 0 give us the field equations. In Einstein-Maxwell theory, they are given as Equations (7) are known as Einstein's field equations, where G µν is the Einstein tensor and T µν is the electromagnetic energy-momentum tensor Also, equations (8) together with ∇ [λ F µν] = 0 are Maxwell field equations in the curved spacetime. Now consider two arbitrary variations δ 1 and δ 2 . Suppose these two variations do not commute δ 1 δ 2 = δ 2 δ 1 . By varying Eq.(6), we find second order variation of the Lagrangian Similarly, one can write By subtracting Eq.(12) from Eq.(11), we have where δ [1,2] = δ 1 δ 2 − δ 2 δ 1 is commutator of two variations δ 1 and δ 2 . By using Eq.(6), and replacing δ → δ [1,2] , we can write Eq.(13) as where is the Lee-Wald symplectic current. Since the symplectic potential is linear in δΦ then the terms containing δ 1 Φ, δ 2 Φ and δ [1,2] Φ eliminate each other and ω µ LW is a skew-symmetric bilinear in δ 1 Φ and δ 2 Φ. The Lee-Wald symplectic current is conserved when equations of motion and linearized equations of motion are satisfied. In other words, if Φ is a solution of E Φ = 0 and δ 1 Φ and δ 2 Φ are solutions of δE Φ = 0, then the Lee-Wald symplectic current is conserved The sign ≃ indicates that the equality is held on-shell. We can define symplectic 2-form on solution space through the Lee-Wald symplectic current where C is a codimension-1 spacelike surface. Solution phase space can be constructed by factoring out the degeneracy subspace of configuration space (see Ref. [12] for detailed discussion). Hence Ω LW will be a symplectic form on solution phase space and it is closed, skew-symmetric and nondegenerate. Suppose ξ µ (x) and λ(x) to be generators of diffeomorphism and U (1) gauge transformation. We can introduce a combined transformation so that χ = (ξ, λ) is the generator of such transformations [17]. The change in metric and U (1) gauge field induced by an infinitesimal transformation generated by χ are given by respectively. Here, L ξ denotes the Lie derivative along the vector field ξ. Also, the change in Lagrangian (4) induced by an infinitesimal transformation generated by χ is Since change in metric and U (1) gauge field are linear in generator χ and change in the Lagrangian is a total derivative then χ generates a local symmetry on solution phase space [12]. The generators of such local symmetry on solution phase space are conserved charges. The charge perturbation conjugate to χ is defined as The algebra among conserved charges is whereC(χ 1 , χ 2 ) is extension term and the Dirac bracket is defined as Now, we want to find explicit form of conserved charges in the Einstein-Maxwell theory. To this end, we assume that the variation in Eq.(6) is induced by an infinitesimal transformation generated by χ then we can define an on-shell Noether current which is conserved on-shell, i.e. ∂ µ J µ N ≃ 0. Thus there exists a second rank tensor density K µν We refer to K µν N as Noether potential and in the given theory it is given by which can be obtained by substituting Eq.(4) and Eq.(9) into Eq. (25). To find explicit form of the symplectic current, first, we take an arbitrary variation from Eq.(25) To have generality we assume that χ depends on the dynamical fields. On the other hand, second variation of Eq.(6), induced by an infinitesimal transformation generated by χ, is Since the commutator of an arbitrary variation and a variation induced by an infinitesimal transformation generated by χ is δδ χ − δ χ δ = δ δχ then the equation (28) can be written as By substituting Eq.(24) into Eq.(29), we find the explicit form of the symplectic current as with In the Einstein-Maxwell theory the explicit form of Q µν LW can be found by substituting equations (26) and (9) into the above equation where h µν = δg µν . The first line in the right hand side of Eq.(32) is the contribution from the gravity part and the second line is the contribution from the U (1) gauge field part in the Lagrangian (4). We can use Eq.(30) and Stokes' theorem to write conserved charge perturbation (21) as where D denotes boundary of C and it is a spacelike codimension-2 surface. Usually it is thought that the linearization is just valid at spatial infinity. To overcome this problem, we take an integration from Eq.(33) over one-parameter path on the solution phase space. To this end, suppose that Φ(N ) is a collection of fields which solve the equations of motion of the Einstein-Maxwell theory, where N is a free parameter in the solution phase space. Now, we replace N by sN , where 0 ≤ s ≤ 1 is just a parameter. By expanding Φ(sN ) in terms of s we have Φ(sN ) = Φ(0) + s ∂Φ ∂s s=0 + · · · . By substituting Φ = Φ(sN ) and δΦ = ds ∂Φ ∂s s=0 into Eq.(33), we can define the conserved charge conjugate to χ. Then we will have where integration over s denotes integration over the one-parameter path on the solution phase space. In the equation (34), s = 0 is the value of the parameter corresponds to the background configuration. In this way, background contribution in the conserved charge is subtracted and then the conserved charge will be always finite. Therefore, this method is applicable to spacetimes with any backgrounds.

III. KERR-NEWMAN (A)DS BLACK HOLE
In this section we briefly review the Kerr-Newman (A)dS black hole geometry (see e.g. [18]) and then we will find the near horizon behavior of this black hole in the Gaussian null coordinates.

A. Geomerty
The Kerr-Newman (A)dS black hole is a solution for the Einstein-Maxwell theory. The metric corresponding to the given black hole in the Boyer-Lindquist coordinate system (t, r, θ,φ) is with Σ = r 2 + a 2 cos 2 θ, where M , a and Q are constants and they parameterize the solution phase space. Also, the gauge field is given by The mass, angular momentum and electric charge of the Kerr-Newman (A)dS black hole are related to M , a and Q as respectively [19]. Spacetime described by metric (35) is stationary and axially symmetric. Strictly speaking, it admits ξ (t) = ∂ t and ξ (φ) = −∂φ. Also, the theory considered in this paper is invariant under U (1) gauge transformation. One can use covariant phase space method to find conserved charges conjugate to symmetry generators. According to the results of previous literature, mass, angular momentum and electric charge are conserved charges conjugate to symmetry generators  [16,17,19]). The steps of calculating mass, angular momentum, electric charge and entropy of Kerr-Newman (A)dS Black Hole are exactly the same as what were done in [16]. Therefore, we refrain from expressing the steps. The equation ∆ r = 0 has at least two real roots r + and r − provided that the parameters M , a, Q, and Λ are chosen suitably. The event horizon is located at r = r + (the largest real root of ∆ r ) and r − is the inner horizon radii. In this way we can rewrite ∆ r in the following form where M and a are related to r + and r − as The above expressions will be reduced to the corresponding expressions for Kerr-Newman black hole when we set Λ = 0.

B. Near horizon behaviour
In order to find near horizon geometry of the Kerr-Newman (A)dS black hole first we write the metric (35) in the advanced Eddington -Finkelstein coordinates (v, r, θ,φ). To this end, we transform coordinates as and we find that Since the horizon velocity is given by Ω H = aΞ r 2 + +a 2 then it is natural that we perform another coordinates transformation asφ = φ + Ω H v. Here index H refers to the Horizon. In this way, we have In this coordinate system the U (1) gauge field can be written as and we have g vv = g vφ = 0 on the event horizon. Now we write near horizon fall-off conditions for Kerr-Newman (A)dS black hole in the Gaussian null coordinate system. To do this, we follow the method proposed in Appendix A of the paper [20]. Therefore, we rewrite the metric relative to the correct set of geodesics. A suitable pair of cross-normalized null normals is These vectors are defined on horizon and we have l · l| H = n · n| H = 0 and l · n = 1. Now we consider a family of null geodesics that crosses H. The vector field tangent to them is n and they are labeled by (v, θ, φ). Suppose ρ is an affine parameter which parameterize the given geodesics so that ρ = 0 on H. The geodesics can be constructed up to third order in ρ: where X µ ρ=0 = (v, r + , θ, φ) and dX µ dρ ρ=0 = n µ . Also, by using geodesic equation n ν ∇ ν n µ | H = 0, one can find the second order derivative of X µ with respect to ρ at horizon The equation (48) defines a transformation from (v, r, θ, φ) to (v, ρ, θ, φ) and then we can calculate the first order expansion of the metric g µν = g here the prime denotes derivative with respect to radial coordinate. Also, κ is surface gravity of the Kerr-Newman (A)dS black hole .
In the new coordinate system, the gauge field can be expanded as We have avoided writing the first order terms in A φ and A θ because we do not need them. From Eq.(50), the full 2-metric on horizon is This metric is conformally related to Riemann sphere. To show this relation, we introduce a field-dependent change of coordinates where µ(θ) is a real function of θ andz is complex conjugate to z. Depending on the sign of cosmological constant, µ(θ) will be different. The explicit form of µ(θ) can be written as where W(θ) is a function of θ and its explicit form depends on the sign of cosmological constant The both Λ > 0 and Λ < 0 cases will tend to Λ = 0 case when l → ∞. Now, we can write the metric of the horizon in the conformal form The conformal factor Ω is a function of z andz. Hence, the metric of the horizon is locally, conformally equivalent to the two-sphere.

IV. NEAR HORIZON FALL-OFF CONDITIONS
In the previous section, we wrote the near horizon metric in the Gaussian null coordinate system. Therefore, following [21], we can consider near horizon fall-off conditions for the Kerr-Newman (A)dS black hole to be where v is the advanced time coordinate such that a null surface is defined by g αβ ∂ α v∂ β v = 0 and the vector tangent to this surface is given by k µ = g µν ∂ ν v which defines a ray. Also, ρ is the affine parameter of the generator k µ . Suppose κ, θ A , Ω AB and λ AB are functions of x A , where two coordinates x A are chosen constant along each ray. Also, one can introduce following near horizon fall-off conditions for the U (1) gauge field where we set A ρ = 0 as a gauge condition and ϕ v , ψ v , ϕ A and ψ A are functions of x A . By substituting fall-off conditions (61) and (62) where Ω AB is the inverse of Ω AB (we explicitly assume that Ω AB is invertible). Since the metric of horizon Ω AB is a Riemannian (not Lorentzian) one, then ϕ v has to be a constant. The other components of the equations of motion relate first order terms to zeroth order ones in metric and gauge field expansions and we do not need them later.

V. NEAR HORIZON SYMMETRIES
The change in metric and U (1) gauge field induced by an infinitesimal transformation generated by χ are given by (18) and (19). Now, we want to find the residual symmetries such that they respect to fall-off conditions (61) and (62). We find that symmetry generator χ with following components preserves the given near horizon fall-off conditions. Here T , Y A andλ are arbitrary functions of x A . In order to obtain the asymptotic symmetry generator χ, we assumed that the leading terms does not depend on the dynamical fields. Under such an assumption the boundary conditions will be "state independent", which means that the form of the asymptotic symmetry generators are not considered to depend explicitly of the charges [23]. The change in dynamical fields under the action of symmetry generator χ can be read as where L Y denotes the Lie derivative along Y A and∇ A is the covariant derivative with respect to connectionΓ A BC compatible with the metric of the horizon Ω AB . It is worth mentioning that because κ and ϕ v are not dynamical then they will remain unchanged under the action of the symmetry generator χ, i.e. δ χ κ = 0 and δ χ ϕ v = 0. The asymptotic Killing vectors (64) are functions of the dynamical fields. To take it into account we introduce a modified version of Lie brackets [22] [ξ 1 , where ξ 1 = ξ(T 1 , Y A 1 ) and ξ 2 = ξ(T 2 , Y A 2 ) and δ (g) ξ 1 ξ 2 denotes the change induced in ξ 2 due to the variation of metric δ ξ 1 g µν = L ξ 1 g µν . Therefore one finds that Thus, the algebra of asymptotic Killing vectors is closed. In addition to T and Y A , the symmetry generator χ = χ(T, Y A ,λ) contains another degree of freedom,λ. Here,λ is an arbitrary function of x A and generates U (1) symmetry. Hence, we need to introduce two other commutators [χ(0, 0, 0,λ 1 ), in addition to Eq.(69). The equation (71) comes from the fact that U (1) is an Abelian group and we will justify Eq.(72) when we consider the algebra among conserved charges. The induced metric on the horizon Ω AB is conformally related to the Riemann sphere and the Laurent expansion on the Riemann sphere is allowed. Since the general solution of the conformal Killing equations is Y = Y z (z)∂ z +Yz(z)∂z and T = T (z,z) andλ =λ(z,z) are arbitrary functions of z andz, we can define modes as where m, n ∈ Z. By using equations (69), (71) and (72), we find the algebra among these modes This algebra contains a set of supertranslations current T (m,n) and two sets of Witt algebra currents, given by Y m andȲ m . It also contains a set of multiple-charges currentλ (m,n) . Two sets of Witt currents are in semi-direct sum with the supertranslations and multiple-charges current. The subalgebra (74) is known as bms H 4 [23,24] and it differs from Bondi-Metzner-Sachs algebra bms 4 [25][26][27](the structure constants are different).

VI. CHARGES AND SOFT HAIRS
Now we are ready to find conserved charge conjugate to the asymptotic symmetry generator χ with components (64) and (65). To this end, we take codimension-two surface D in Eq.(33) to be the horizon By substituting the boundary conditions and components of the asymptotic symmetry generators into Eq.(76), we have where an integral over one-parameter path on solution phase space was taken. As we mentioned earlier, one can use equations (22) and (23) to find the algebra among the conserved charges. After performing some calculations, we find that where equations (66) and (67) were used also [χ 1 , χ 2 ] is given by equations (69)-(72). In this case, by comparing Eq. (22) and (78), we see that the central extension term does not appear. Since the algebra among the conserved charges is isomorphic to algebra among symmetry generators and the commutation relation (72) is appeared in the right hand side of Eq.(78) then it seems reasonable to consider such a commutation relation. By substituting Eq.(73) into Eq.(77), supertranslation, superrotation and multiple-charge modes can be obtained as respectively, where γ = det(γ AB ). Also, the equation (78) gives us the algebra among these modes Now we apply the above considerations on the Kerr-Newman (A)dS black hole. Consequently, we can obtain charge zero-modes explicitly and then interpret them. Since (z,z) coordinates are related to (θ, φ) coordinates through the equation (56) and then we can easily read supertranslation charge modes as where Hence, the supertranslation double-zero-mode charge T (0,0) is where I(0) = 2 was used. The entropy of the Kerr-Newman (A)dS black hole is given by (see e.g. [19]) then the supertranslation double-zero-mode charge T (0,0) is equal to the the Kerr-Newman (A)dS black hole entropy multiplied by Hawking temperature T H = κ/2π, as expected [23,24,28]. Similarly, multiple-charge modes are with W (m) =ˆπ 0 (r 2 + − a 2 cos 2 θ) (r 2 + + a 2 cos 2 θ) 2 µ(θ) 2m sin θdθ.
where ψ v = A (1) v was used. One can show that the multiple-charge double-zero-mode gives the Kerr-Newman (A)dS black hole electric charge Now we calculate superrotation charges. θ z and θz are related to θ θ and θ φ as These relations are deduced from the fact that θ z dz + θzdz = θ θ dθ + θ φ dφ. Also, we have θ θ = g (1) vθ and θ φ = g (1) vφ . Therefore, the explicit form of the charges associated to superrotations are and it does not provide inner horizon entropy of the Kerr-Newman (A)dS black hole (however, for Kerr black hole it does). This result is independent of the choice (109). The chirally symmetric sum of zero modes isĴ where is the horizon electric potential. Thus, we have shown that the Kerr-Newman (A)dS black hole entropy is bilinear in the zero modes and it satisfy the new entropy formula S = 4πĴ + 0Ĵ − 0 proposed in [11]. It is also clear from Eq.(108) that the angular momentum is given by

VIII. CONCLUSION
We have briefly reviewed the approach of the covariant phase space method of obtaining conserved charges in Einstein-Maxwell theory. According to [17], we introduced combined symmetry generator χ = (ξ, λ), which consists of diffeomorphism and U (1) gauge transformation. The covariant phase space method presented in section II, is not only applicable to the asymptotic symmetries at spatial infinity but also it is applicable to the near horizon asymptotic symmetries. In section III, we have briefly reviewed the Kerr-Newman (A)dS black hole geometry and then we found the near horizon behavior of this black hole in the Gaussian null coordinate system. We showed that the induced metric on the horizon is conformally related to the Riemann sphere. Therefore the Kerr-Newman (A)dS black hole horizon admits conformal symmetry. The explicit form of conformal factor Ω = Ω(z,z) depends on the sign of cosmological constant (see Eq.(58) and Eq.(60)). Therefore, we expect that fall-off conditions near the isolated horizon in the Einstein-Maxwell theory are given by Eq.(61) and Eq(62), where κ and ϕ v are constants (imposed by field equations). These fall-off conditions are preserved by the action of asymptotic symmetry generators χ (components of χ are given by Eq.(64) and Eq.(65)). Equations (69)-(72) give the algebra among these asymptotic symmetry generators. Because the algebra among the conserved charges and the asymptotic symmetry generators must be isomorphic, the additional commutation relation (72) was introduced. The asymptotic symmetry generator modes, satisfy an algebra contains of a set of supertranslations current T (m,n) , two sets of the Witt algebra currents, given by Y m andȲ m , and a set of multiple-charges currentλ (m,n) . Two sets of the Witt currents are in semi-direct sum with the supertranslations and multiple-charges current. In section VI, we found conserved charges conjugate to these modes. The supertranslation double-zero-mode charge T (0,0) gives the Kerr-Newman (A)dS black hole entropy multiplied by Hawking temperature. Also, the multiple-charge double-zero-mode gives the electric charge of the Kerr-Newman (A)dS black hole. One expect that the zero-mode charges associated to superrotations give angular momentum of black holes. But it is not true when black hole have electric charge (See equations (94) and (95)). Due to the presence of second terms in the right hand sides of Eq.(94) and (95), this problem occurs when one considers just diffeomorphism generated by Y A . To cure this problem, we must consider both diffeomorphism and U (1) gauge transformation together. To do this, we introduced a transformation generated by χ(Y ) = χ(0, Y A ,λ(Y )) → Y , whereλ is a function of Y A and it does not generate an independent symmetry. We defined corresponding zero modes as Y . By a gauge fixing asλ = Y A ϕ A , we have found charges conjugate to these modes. The zero mode charges