Non-analyticity of holographic Rényi entropy in Lovelock gravity

We compute holographic Rényi entropies for spherical entangling surfaces on the boundary while considering third order Lovelock gravity with negative cosmological constant in the bulk. Our study shows that third order Lovelock black holes with hyperbolic event horizon are unstable, and at low temperatures those with smaller mass are favoured, giving rise to first order phase transitions in the bulk. We determine regions in the Lovelock parameter space in arbitrary dimensions, where bulk phase transitions happen and where boundary causality constraints are met. We show that each of these points corresponds to a dual boundary conformal field theory whose Rényi entropy exhibits a kink at a certain critical index n.


Introduction
We consider a quantum field theory in a d-dimensional Minkowski spacetime when at t = 0 the system gets separated in two parts, A and its complement B, by a (d − 2)-dimensional hypersurface Σ. A legitimate question to ask is how much the degrees of freedom in the two sub-systems A and B are correlated. Entanglement entropy (EE) and the Rényi entropy (RE) are important measures of this quantum correlation. In particular EE across the entangling surface Σ is given by where ρ A is the reduced density matrix of the sub-system A, i.e. the density matrix obtained after integrating out the degrees of freedom in B [1][2][3][4]. The n-th RE, with n ≥ 0, associated with a quantum system described above is defined as S n = 1 1 − n ln tr (ρ n A ) . (1. 2) The whole set of eigenvalues of the reduced density matrix ρ A can be reconstructed by knowing the RE for all the indices n. For CFT's in flat space, RE exhibits a universal relation to the central charges of the theory, in particular the derivative of RE with respect to n evaluated at n = 1 is proportional to the coefficient of the stress tensor two-point function [5,6]. Moreover, in the limit where n → 1 RE reduces to EE. In general, RE and EE are rather difficult to compute and measure, although remarkable progress in this direction has been made recently [7][8][9]. In quantum field theory RE is mainly computed by means of the so-called replica method [1,[10][11][12]. Here, one replaces the computation of the n-th power of the density matrix (and thus the corresponding partition function) with that of the density matrix of a theory which consists of n copies of the original quantum field theory. This amounts to computing the Euclidean partition function JHEP08(2017)002 on a geometry with conical singularity. Although a direct "holographic translation" of the replica approach might involve conically singular geometries, which are generally difficult to deal with and may not lead to the correct results [13,14], RE can be studied holographically.
In holographic theories EE can be computed by the Ryu-Takayanagi (RT) formula 1 involving minimal surfaces which extend into the bulk and end on the boundary entangling surface [18][19][20]. A somewhat similar prescription for RE has been provided only recently in [21]: RE can be determined by computing the area of cosmic branes which back-react with the bulk geometry. Despite its beauty and geometric foundation, the prescription in [21] can be arduous to handle in general cases.
Another remarkable approach to compute holographic EE for spherical entangling surfaces is the one proposed by Casini, Huerta, and Myers (CHM) [22], extended to the holographic RE in [23]. It consists of a conformal mapping on the CFT which takes us from an Euclidean conically singular geometry to an Euclidean smooth thermal hyperboloid. The gravity dual of such a thermal CFT (if it exists) is a black hole with hyperbolic event horizon in asymptotically AdS (AAdS) spacetimes. Hence, the CHM map relates the RE of the original CFT to the free energy of AAdS hyperbolic black holes. The index of the RE is translated into the inverse of the black hole temperature (compared to some reference temperature). Therefore, the knowledge of RE at any n (quantum entanglement spectrum) requires the knowledge of free energy (and thus thermal entropy) of a hyperbolic black hole in AdS at any temperature. We will review the crucial steps of the CHM map in section 2.
The advantages of CHM approach are twofold. First of all, it avoids conical singularities and related problems [13,24], by working on a thermal ensemble which makes the boundary geometry perfectly smooth and straightforwardly treatable via standard holographic techniques. Second, it applies to any gravity theory (assuming they have a CFT dual) and in particular to higher derivative gravities [23,[25][26][27][28], unlike the RT formula which needs to be corrected [29][30][31][32][33][34][35].
In this manuscript we apply the CHM approach to study RE of holographic CFT, dual to higher derivative gravity theories, in particular the so-called third order Lovelock gravity [36,37], in an asymptotically AdS spacetime. Lovelock gravities are interesting generalizations of Einstein gravity, which are ghost-free and living in dimensions (strictly) greater than four with small coupling constants, i.e. small corrections to general relativity. In third order Lovelock gravity the Einstein-Hilbert action is corrected with terms proportional to R 2 (with R the curvature scalar), also known as Gauss-Bonnet gravity, 2 and R 3 with dimensionless coupling constants λ and µ, respectively. We will review basic aspects of Lovelock gravity in section 3.1. These theories have proven useful in exploring various properties of holographic theories, as for example the viscosity bounds [40][41][42], although at intermediate energy scales they might become problematic [43]. 3 However, in this work we always assume that Lovelock couplings are small positive numbers, satisfying constraints 1 The formula has recently been proved in [15,16], a first attempt to prove it was presented in [13], cf. [17] for a recent review on holographic EE. 2 For the relation between Gauss-Bonnet gravity and string theory see for example [38,39]. 3 "Intermediate energy scales" is referred to energy scales where higher derivative corrections are important but the theory is still weakly coupled [43].

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coming from boundary causality [44], as will be reviewed in section 3.2. We work in a classical regime, therefore, the necessary additional degrees of freedom mentioned in [43] to cure causality are not relevant to our discussions. As we will see in section 3.3 third order Lovelock theories reveal interesting and unusual features, not present in Einstein gravity and not even in Gauss-Bonnet gravity. Our study unveils first order phase transitions between coexisting hyperbolic black holes in third order Lovelock gravity. Such phase transitions were originally observed in a study by one of the authors in [45], however, only for the special case where µ = λ 2 /3. In the present work, by exploring the complete Lovelock parameter space spanned by {λ, µ}, we find that in any given dimension, there are regions where the hyperbolic black holes with smaller mass are favoured at low temperature. Some of these phase transitions are in the range of parameter space which is excluded by boundary causality, including the specific case µ = λ 2 /3. Nevertheless we can still observe plenty of phase transitions in the causal regions. Figure 3 shows an example of regions where causality and bulk phase transitions overlap in 7, 8 and 9-dimensions. For instance, in seven dimensions (d = 6) we observe phase transitions in the causal range for 0.25 ≤ λ ≤ 0.387 and 0.024 ≤ µ ≤ 0.105, or in terms of actual Lovelock couplings, for 0.021 ≤ α 2 L 2 ≤ 0.032 and 0.001 ≤ α 3 L 4 ≤ 0.004. Note that, in the causal range where phase transitions happen the Lovelock couplings in (3.1) are still small enough that L 2 and L 3 can be considered as perturbations to the Einstein term.
Furthermore, the first order nature of the phase transitions indicates a discontinuity in the black hole thermal entropy. As mentioned earlier in CHM holographic approach, the RE of a boundary CFT is related to the free energy, and thus to the thermal entropy of black holes. It is then interesting to investigate the effects of these bulk phase transitions on the boundary field theory RE. This is the main focus of this work and the results are discussed in section 4. The holographic RE for third order Lovelock gravity was already computed in [23,25]. The novelty here is to take into account that such black holes undergo phase transitions, to systematically span the causal parameter space, and analyse the consequences for the dual RE. Connections between RE and bulk phase transitions have been previously studied in [46,47]. However, there are two main differences here. First of all, our system is purely gravitational, dual to a CFT in its vacuum state with the only corrections coming from the corrections of the coupling constants. In [46] the authors holographically computed RE by considering Einstein gravity with the addition of a scalar field (similarly in [47] for the case of a charged system), and the instability of hyperbolic black holes is due to the development of hair. Second, our phase transition is first order, while in [46,47] it is second order. This has a crucial effect on the RE: our results show that for strongly coupled dual CFT's the RE displays a kink at a critical index n which results in the non-analyticity of RE with respect to n nearby the kink.
While our findings are particularly interesting for d = 6 where we have known examples of AdS/CFT dualities, they are valid as well for d-dimensional field theories with d > 6. In fact, from the bulk point of view the number of dimensions D = d + 1 is a mere parameter, and it is interesting to explore its effect on the system. Our analysis shows that D = 7 is not special: in any dimension D = d + 1 ≥ 7 it is possible to find regions of the JHEP08(2017)002 parameter space where black holes are unstable and where the would-be boundary field theory is causal (even though these regions shrink as we increase the number of spacetime dimensions). Existence of higher (d > 6) dimensional CFT's is still an open question, e.g. [48]. However, assuming that a dual CFT exists, here third order Lovelock theories can serve as a toy-model: they allow us to straightforwardly carry on computations, and thus, to explore the role of higher derivative gravity in this context. This kind of approach has turned out to be helpful in the past, e.g. cf. [40][41][42] on the discussion of the viscosity bound or [31,32] for the discovery of the F-theorem. For this reason, we hope that the holographic system studied in this work might be instructive to predict novel features for strongly coupled higher dimensional conformal field theories.

Holographic Rényi entropy
We will be interested in thermal states, so it is useful to understand the role of Rényi entropies in this case. A description of the quantum Rényi entropy for a thermal state in terms of the free energy has been discussed in [49]. Suppose we have a physical system which is in thermal equilibrium at temperature T 0 . When the system is "quenched" and the temperature is lowered by a factor n, the Rényi entropy is a measure of the maximum amount of work (divided by the difference of temperature) the system can do in reaching the new equilibrium state and is given by In the limit n → 1 the right hand side of expression (2.1) gives the usual relation for thermal entropy, i.e.
which can be then used to rewrite the Rényi entropy in (2.1) as We now review the main steps of the CHM approach to compute holographic Rényi entropy [22,23]. Let us start with a CFT in R 1,d−1 in the vacuum state. The system is at zero temperature, and we introduce a (d − 2)-dimensional spherical entangling surface Σ. The conformal transformations found in [22] map the reduced density matrix of a CFT in flat spacetime to a thermal density matrix of a CFT on a hyperbolic geometry The radius of the curvature of the hyperbolic plane matches the radius R of the entangling surface Σ, and JHEP08(2017)002 in particular the temperature is given by the inverse of R. 4 The mapping among density matrices extends to the entropy. Hence, the entanglement entropy of a spherical entangling (d − 2)-dimensional surface of radius R in a CFT in flat spacetime is equivalent to the thermal entropy of a CFT at temperature T 0 = 1/2πR in a hyperbolic geometry R × H d−1 .
According to the AdS/CFT correspondence, a thermal state in the boundary CFT is dual to a black hole in the bulk geometry. Since the CFT has been defined on a hyperbolic plane, by matching the geometry on both sides of the duality, the appropriate black hole to consider in the bulk is the so-called topological black hole, i.e. one with hyperbolic horizon [22]. The Hawking temperature of the black hole is then related to the temperature of the dual field theory according to the usual AdS/CFT dictionary. Therefore, in this framework, the entanglement entropy across Σ is given by the horizon entropy of a hyperbolic AdS black hole [22].
The procedure described above can be extended in a straightforward manner to the holographic calculation of Rényi entropies for a spherical entangling surface [23,25]. We have seen above that the computation of Rényi entropies requires the knowledge of the system at a temperature T given by T 0 /n, see for example (2.1). Holographically, this means that we need to extend the AdS hyperbolic black hole solution to any T = T 0 /n.

Thermodynamics of Lovelock black holes
In section 3.1 we recall some basic features of third order Lovelock gravity with a negative cosmological constant and the corresponding hyperbolic black hole solutions. In section 3.2 we review the constraints on the Lovelock coupling constants {λ, µ} imposed by requiring that the boundary CFT is causal. In section 3.3 we study the thermodynamics properties of these black holes as a function of the couplings in arbitrary dimensions.

Topological Lovelock black holes
In a spacetime with dimensions higher than four, Einstein gravity is not the most general gravitational theory sharing the basic properties of standard general relativity, that is field equations are generally covariant and contain at most second order derivatives of the metric. Based on these assumptions, the action for the most general gravity theory in (d + 1)-dimensions is written as Lovelock gravity with the Lagrangian in the form [36,37] where L 1 is the Einstein-Hilbert term, L 2 is the Gauss-Bonnet term, L 3 is a third order Lovelock term, and so on. Here, we consider up to third order Lovelock gravity with a 4 The conformal transformations found in [22] map the causal development of the region inside Σ to a Rindler wedge, which is in turn mapped to a hyperbolic plane H ≡ R × H d−1 . The crucial point is that the vacuum state of the original CFT is mapped to a state in H which looks thermal with respect to the Hamiltonian generating the time evolution in H (we refer the reader to the original reference [22] for more details), hence the relation among the density matrices.

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negative cosmological constant, therefore we restrict ourselves to the following action where R is the curvature scalar in the bulk, and L is the scale of the cosmological constant described by the first term in (3.1), p is the Plank length, α 2 and α 3 are the second and third order Lovelock couplings with dimensions of a (length) 2 and (length) 4 , respectively. 5 L 2 and L 3 are not zero only for dimensions strictly higher than four and six, respectively. They are simply proportional to the corresponding Euler density in four and six dimensions. For convenience, the Lovelock coefficients are written in terms of dimensionless parameters as follows .
Here λ and µ are chosen to be positive. By varying the action (3.1), one obtains the equations of motion up to third order in Lovelock coefficients as follows We will consider spherically symmetric hyperbolic black holes, thus we can employ the following metric ansatz where dΣ −1,d−1 is the metric of a (d − 1)-dimensional unit hyperboloid and N is a constant introduced to have a convenient normalization of the time coordinate. Clearly, h(ρ) has JHEP08(2017)002 to be a solution of the equations of motion (3.5). Plugging the ansatz (3.8) into the equations (3.5), we obtain a simple expression for the integral of motion Note that m is the dimensionless black hole conserved charge, therefore a measure of its mass. m (3.9) can be expressed in terms of the (dimensionless) black hole horizon ρ H , defined by g tt (ρ H ) = 0, that is Similarly, the integral of motion (3.9) evaluated at the boundary ρ → ∞ defines the asymptotic value of h(ρ), i.e. h ∞ , as 12) in this way the curvature scale of the hyperbolic spatial slices is R in the boundary CFT on R × H d−1 . The metric (3.8) asymptotically represents a pure AdS spacetime with radius L where 13) or in other words, the effective cosmological constant is, in fact, (3.14) In principle, equation (3.11) could have three real distinct solutions provided the discriminant is positive. Therefore there exist three different effective cosmological constants. However, if the discriminant of (3.11) vanishes, all three solutions coincide. This happens at λ = 1/3 and µ = 1/27, thus the theory has maximum degeneracy and the full symmetry of AdS is recovered for this particular choice of Lovelock parameters. By examining the equations of motion (3.9), it is straightforward to find that there is always a unique solution for h(ρ) which is real everywhere provided that, in any given dimension, the Lovelock coefficients satisfy the following condition From this point forward parameters are chosen such that the condition (3.15) holds. Also the discriminant of (3.11) is strictly negative when the inequality in (3.15) is fulfilled and therefore a fixed {λ, µ} results in only one effective cosmological constant, i.e. a unique AdS at the boundary. The metric solution for generic λ and µ is easily obtained from equation (3.9) as 6 . 6 We partly borrow notation used in [45].

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In the following we also express other thermodynamic formulae which will be used to aid in further calculations. 7 One can assume a black hole as a thermodynamic system [50][51][52][53] and define the Hawking temperature [54,55] as With our conventions, the AdS solution corresponds to a temperature given by . (3.18) This can be seen by using the relation (3.10) with m = 0, and recalling that for an AdS The ADM mass can be worked out in a straightforward manner from m (3.10), and it is given by where V Σ is the volume of the hyperboloid Σ −1,d−1 . The horizon entropy can be computed from the Wald entropy formula [56][57][58], and it results in [25] V Σ is a divergent quantity, and in particular its leading behaviour is proportional to 2−d , where is a short-distance cut-off [22,23]. Such UV-divergences are expected, and they correspond to the (divergent) terms responsible for the so-called area law in the boundary field theory. In a classical regime the bulk partition function reduces to the exponential of (minus) the regularized classical on-shell action S E,reg , thus the black hole free energy is simply given by F = T S E,reg . (3.21) S E,reg can be computed by extending holographic counter-term methods to general Lovelock theories, explicitly developed in [59,60] and initiated in [61][62][63]. 8 The final result can be written as where M , T , and S are given by (3.19), (3.17), and (3.20) respectively. E 0 is a finite constant term which arises from the counter-term methods, and accounts for the Casimir energy. It depends upon the Lovelock couplings {λ, µ}, but not on the horizon data. 9 Consequently, it leads to an overall shift in the free energy. 7 We do not follow the conventions adopted in [23,25], however our results if written in terms of the parameter x, i.e. x = ρH √ h∞ , agree exactly with theirs. 8 For an alternative regularization approach to derive similar counter-terms, we refer an interested reader to [64]. 9 In particular when λ and µ are set to zero E0 reduces to the hyperbolic AdS Casimir energy [65][66][67][68].

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Since we will be interested in comparing free energies of coexisting black hole solutions at any given {λ, µ} and d (section 3.3), the Casimir energy E 0 will not play any role, and we can safely work with the following free energy density per unit volume Here, we introduce the thermal entropy density which will be useful later, as where S is the thermal entropy (3.20). Note that F and S are dimensionless.
In the rest of this section we will investigate the thermodynamics of hyperbolic black holes in the full parameter space {λ , µ} of third order Lovelock gravity in arbitrary dimensions. In particular, we find that in any given dimension for certain values of {λ , µ} there exist multiple isothermal black holes, a fact that is a signal of a possible phase transition in the theory. However, before moving to identify where in the parameter space the phase transition will occur, crucial limits on {λ , µ} should be taken into account which arise from the causality constraints of the CFT boundary theory. These constraints will be briefly discussed in the following section 3.2.

Causality constraints on the Lovelock parameters
Demanding causality of the boundary theory, the fact that the velocity of any signal propagating on the boundary should not exceed the speed of light, will introduce constraints on the Lovelock parameters. These constraints have been well studied in the literature for Gauss-Bonnet [41,[69][70][71][72][73] and third order Lovelock gravities [42,44,74]. Here, we follow the results obtained in [44] for third order Lovelock gravity where the constraints have been derived using the perturbations of metric as well as shock waves calculation. While we encourage an interested reader to find the details of calculations in [44] and reference therein, we only express the final results here. In general, there exist three modes propagating on the boundary: helicity 2, helicity 1 and helicity 0 gravitons. The requirement that each mode propagates with the velocity lower than the speed of light imposes the following constraints: helicity 0 : where h ∞ is governed by equation (3.11).
Exploring the space of Lovelock parameters while respecting constraints (3.25), one finds that the causality of helicity 2 boundary gravitons will set a lower bound on the parameters while the causality of the other two modes imposes an upper bound on the allowed region of {λ, µ}. However, helicity 0 constraint is always more stringent than helicity 1. Therefore, at the end, the allowed region due to causality is identified by the helicity 2 and helicity 0 modes. This is true in any arbitrary dimension.
The shadowed blue region in figure 1 shows the region in the parameter space fulfilling the causality constraints (3.25), as well as reality constraints, in 7, 8 and 9-dimensions, respectively. Recall that in any given dimension, the full metric solution (3.8) is real everywhere whenever the condition (3.15) holds, i.e. µ ≥ λ 2 /3. Therefore any region below the parabola µ = λ 2 3 is excluded although it may be allowed by boundary causality. Figure 1 clearly indicates that the allowed region grows as we move to higher dimensions.

Phase transitions for µ ≥ λ 2 /3
This section is devoted to determine where in the parameter space {λ, µ} of third order Lovelock gravity, phase transitions happen for hyperbolic black holes in arbitrary dimensions. In order to identify whether a thermal phase transition would occur, we need to look for the existence of isothermal black hole solutions. To do so, one should examine the behaviour of the temperature as a function of black hole mass, i.e. T (M ). If we find that temperature is a non-monotonic function of mass, then at a given temperature there are coexisting black hole solutions with different masses, or different horizon radii, which signals the possibility of a thermal phase transition in the gravitational system. In order to confirm that a phase transition happens, one should further compare the free energy of isothermal solutions. The way to investigate non-monotonicity of T (M ) is to examine whether dT dM has a real solution or not: if the derivative has no real solution, temperature is a monotonic function of mass, otherwise is non-monotonic and isothermal solutions exist. Since the ADM mass M (3.19) is proportional to m (3.10), and the black hole temperature and mass m are expressed in terms of the horizon radius in equations (3.10) and (3.17), it is preferred to study dm dρ H and dT dρ H rather than dT dM directly.

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In general, our analysis reveals that non-monotonicity of T (M ) is due to having either two extremal black holes or extrema in the temperature. The former is related to the behaviour of dm dρ H (this simply follows from the thermodynamic relation dM dρ H = T dS dρ ), while for the latter one should inspect dT dρ H . For any d > 6, in order to find the solutions of the equation dm dρ H = 0 at a non-trivial horizon radius ρ H = 0, we need to analyse a cubic equation in terms of ρ 2 H , i.e.
The equation (3.27) should be solved numerically in arbitrary dimensions, except for d = 6 where one can find solutions analytically. The above analysis also applies to the 7-dimensional case (d = 6). However, in this case equation (3.26) is independent of µ. Therefore, the behaviour of dm dρ H for a given λ is valid for all µ's, and here the only constraint on µ is that of the reality constraint, i.e. µ ≥ λ 2 /3. Instead, the behaviour of dT dρ H still depends on both parameters {λ, µ}. To summarize, for a given λ (d ≥ 6) and µ (d > 6) in order to specify non-monotonicity of T (m) due to having two extremal black holes not only the discriminant of (3.26) should be positive but also m ext 1 ≤ m ext 2 . Alternatively, for a given {λ, µ} in any dimension T (m) could be non-monotonic as dT /dρ H = 0 might have more than one real solution.
To proceed further it is beneficial if we classify regions of λ as below: where λ c is obtained by solving equation (3.26) for µ = λ 2 c /3 while demanding m ext 1 = m ext 2 . 10 For any λ < λ c and µ ≥ λ 2 /3 there is only one extremal black hole with m = m ext 2 and horizon radius at ρ H> which is the largest real root of the equation (3.26). Temperature is a monotonically increasing function of mass and therefore, no phase transition is expected in this range.  where a phase transition between two isothermal black holes with different masses occurs at T c ≈ 0.056; on the right for 1/3 < λ < λ d = 3/5 and µ > µ c2 where a phase transition between two isothermal black holes with different masses occurs at T c ≈ 0.292. (b) Thermal entropy density S (3.24) against temperature T /T 0 where the phase transition between two black holes in the lowest and highest branches are shown with black dots. The dashed red line indicates the temperature of phase transition and discontinuity in the thermal entropy reveals that the phase transition is of first order. II) λ c ≤ λ < 1/3: in this region for any λ 2 /3 ≤ µ ≤ µ c 3 the discriminant of equation (3.26) is positive and m ext 1 ≤ m ext 2 , therefore the system has two extremal black holes and T (m) is non-monotonic. For a given λ one can easily obtain µ c 3 by solving equation (3.26) while demanding m ext 1 = m ext 2 . Note that µ c 3 → ∞ in 7-dimensions since equation (3.26) is independent of µ. Thus, in this range of {λ, µ} it is legitimate to expect a phase transition between smaller and larger isothermal black holes at some critical temperature T c ≥ 0. In order to check whether the phase transition happens or not, one should compare the free energy of the black hole solutions against temperature, i.e. F (T ). On the left panel, figure 2a shows such an example where the occurrence of a phase transition is vivid at T c ≈ 0.056. Moreover, by examining black hole entropy S(T ) one finds that the phase transition is of first JHEP08(2017)002 order, see figure 2b on the left panel. Note that for λ = λ c or µ = µ c 3 a phase transition happens at T c = 0, whereas T c increases by increasing λ (or decreasing µ) keeping fixed µ (or fixed λ). Furthermore, as the number of spacetime dimensions becomes larger, λ c approaches 1/3.
in any higher dimension (d > 6). Depending on the value of µ there might exist isothermal black holes due to having either an extremum in the temperature or two extremal black holes. Therefore, one should inspect non-monotonicity of temperature by examining both dT dρ H and dm dρ H . Our analysis indicates that T (m) is non-monotonic in two intervals: λ 2 /3 ≤ µ ≤ µ c 1 and µ c 2 ≤ µ ≤ µ c 3 . For a given λ both µ c 1 and µ c 2 are obtained by demanding that two real non-trivial solutions of equation (3.27) coincide. Whereas µ c 3 for d > 6 is obtained by solving equation (3.26) while demanding m ext 1 = m ext 2 . In 7-dimensions (d = 6) there is no upper bound in the second interval since equation (3.26) is independent of µ. As a result, non-monotonicity of temperature and possible phase transitions are expected in these two intervals. Again, in order to check the actual occurrence of phase transitions, one has to compare the free energy of coexisting solutions. An example of such comparison is shown on the right in figure 2a in 7-dimensions, while the discontinuity of entropy indicates a first order phase transition on the right in figure 2b. It is straightforward to work out similar comparisons of free energy in arbitrary dimensions to see that phase transitions between smaller and larger black holes always happen in the range where temperature is non-monotonic.
The point (λ, µ) = (1/3, 1/27) is an exception in this range as the symmetry enhances the spacetime to a full AdS space for which no phase transition happens.
IV) λ ≥ λ d : in this region the discriminant of equation (3.26) is strictly negative which results in having only one extremal black hole for all values of µ. Therefore, the temperature could only be non-monotonic due to having an extremum which happens if λ 2 /3 ≤ µ ≤ µ c 1 . Again µ c 1 is obtained by demanding that two real non-trivial solutions of equation (3.27) coincide. Then, we expect a possible phase transition in this range and comparing the free energy of isothermal black holes confirms the occurrence of a phase transition, which is first order as other regions. In dimension less than 9, λ d is larger than the maximum λ allowed by causality. Furthermore, λ d approaches to 1/3 as d increases. absent in 7-dimension, since equation (3.26) is independent of µ for d = 6, as we explained above. From figure 3 it is also evident that as dimensionality increases, the red areas in the shaded blue regions (that is allowed by causality) shrink and eventually disappear as d → ∞ since in this limit both λ c , λ d approach to 1/3. This means that we approach to the green dot in parameter space as d → ∞, and no phase transition happens at this point. In another words, the theory is stable for a wider range of Lovelock parameters in higher dimensions.

Results and discussion
We can now investigate the implications of the instabilities of third order Lovelock black holes studied in section 3.3 on the Rényi entropies. As explained in section 2, in order to calculate the Rényi entropy of a boundary CFT, we can either use the expression (2.4), where now S thermal is the black hole thermal entropy in the bulk as a function of its temperature given by expressions (3.20) and (3.17), or we can use (2.1) where now F is the black hole free energy (3.22) again as a function of the temperature (3.17). Let us consider for example the expression (2.4). Recall that T 0 is the temperature of the boundary CFT, and we use this value as a reference temperature, while the final temperature is given by T 0 /n. Keeping fixed T 0 , whenever the final temperature is smaller than T c , we end up integrating over a piece-wise continuous function S thermal . This becomes clear by looking at figure 2b. Thus, the integral over the jump between the two stable branches will result in a continuous but not differentiable function of T T 0 , and this is nothing but the Rényi entropy, cf. (2.4). Figure 4 shows the Rényi entropy in terms of the index n(= T 0 T ) in 7-dimensions for a fixed µ = 0.055 and several λ's, all in the causal region where the phase transition happens in the bulk. It is evident that there is a kink in the Rényi entropy at n c = T 0 Tc which is a direct consequence of the bulk first order phase transition. In particular, in any dimension the kink is placed at n c > 1. This is due to the fact that the phase transitions in the causal regions occur at a critical temperature that is always smaller than T 0 , i.e. Tc T 0 < 1. As expected from field theoretical computations, Rényi entropies are divergent when the index n approaches to zero (in terms of the entanglement spectrum this limit represents the logarithm of the number of non-vanishing eigenvalues), specifically the leading divergence behaves as 1 n d−1 . On the other side, they approach a constant as n → ∞ JHEP08(2017)002 (which is proportional to the logarithm of the largest eigenvalue), where again the specific value of the constant depends on the dimension d and the coupling constant {λ, µ}, see for example the discussion in [23].
In general, in a given dimension for a fixed µ, decreasing (increasing) λ leads to an increase (decrease) in n c . There is always a lower bound on λ given by λ c for which n c → ∞: recall that for λ = λ c the phase transition happens at Tc T 0 = 0 (cf. region II in section 3.3). Moreover, λ ≤ λ max (for a fixed µ) which imposes a lower bound on n c , namely n c min : depending on the value of µ the upper limit λ max is either dictated by causality constraints (3.25) or is the maximum possible λ in the causal region for which a phase transition happens. Figure 5 shows n c min in 7-dimensions for 0.03 ≤ µ ≤ 0.074 and the corresponding λ max which is partly obtained by causality constraints: helicity 2 in the region 0.03 ≤ µ ≤ 0.0405 and helicity 0 for 0.0499 ≤ µ ≤ 0.0741. However, in the range 0.0405 < µ < 0.0499, λ max is the maximum value in the causal region for which phase transitions happen and it belongs to the curve µ c 2 in figure 3 for 7-dimensions. Notice that there is a discontinuity in n c at µ = 0.0406 due to the jump in λ max from the helicity 2 curve to the µ c 2 curve in figure 3. Also in figure 5 the lowest value of n c min = 1.38 (for µ = 0.0406 and λ max = 0.343) indicates that for any fixed µ in 7-dimensions n c ≥ 1.38, i.e. the kink does not happen at or very close to 1. Therefore, despite having a kink the Rényi entropy is still smooth and differentiable in the vicinity of n = 1.
Alternatively, in a given dimension one can examine how n c varies with µ for a fixed λ: our analysis reveals that n c increases (decreases) with increasing (decreasing) µ. Therefore, for each λ the minimum value of n c , namely n c min , is obtained for the minimum µ in the causal region for which the phase transition happens. From figure 3 it is easy to see that in 7-dimensions µ min is partly obtained by causality constraints, in particular by the helicity 2 constraint for λ c ≤ λ ≤ 0.343 and by the helicity 0 constraint for 0.364 ≤ λ < 0.389. Whereas µ min belongs to the curve µ c 2 if 0.343 < λ < 0.364. One can reproduce a plot JHEP08(2017)002 similar to 5 for n c min but at a fixed λ and correspondent µ min . However, the lowest value of n c is still n c min = 1.38, obtained for λ = 0.343 µ min = 0.0406. Hence, we have again that n c ≥ 1.38 and the kink is far enough from n = 1 to give a differentiable Rényi entropy in the vicinity of n = 1.
To our knowledge this is the first pure gravitational system to produce first order phase transitions in the bulk which are reflected in a kink of the dual Rényi entropy. In holographic field theories, second order phase transitions were previously discussed in [46,47]. 11 There, the second derivative of the Rényi entropies with respect to the index n was found to be discontinuous. We stress that there the bulk mechanism to give arise the phase transition is rather different: it is either due to the formation of hairy black holes in presence of light scalars [46] or due to a holographic superconductor-like mechanism in the charged case [47]. Our original boundary field theory is a CFT at zero temperature living in a flat d-dimensional space where we have a bipartite system separated by a (d − 2)-dimensional spherical entangling surface of radius R. The only scale present here is set by the radius of the entangling surface. We are essentially probing the ground state of this bipartite system. Our results suggest that there is an emergent critical index n c (where the Rényi entropy displays a kink) which might be a sign of a phase transition in the ground state: that is the spectrum seems to have distinct regions, likely characterised by two distinct probability distributions.
An analogous non-analytic dependence was found in the universal coefficients of Rényi entropy for the O(N ) model close to critical points [77] (both in the large N -limit and 4− -expansion). 12 This was found by purely field theoretic considerations but O(N ) vector models are conjectured to be dual to higher spin theory in AdS [78,79], 13 suggesting that similar behaviours to that found in our study can also been seen in another gravitational setting. Another field theoretical example is provided by the work [81]. Here, the authors find a phase transition in the Rényi entropy for Luttinger liquids at a critical n c , which emerges essentially when the index n has a significant effect on the natural scale of the field theory (Luttinger parameter). An important lesson from [81] is that the replica method would miss such a phase transition, and a general caution should be kept in mind in applying the replica method in cases where Rényi entropy is not analytical. Nevertheless, as already pointed out in [47] the fact that Rényi entropy might not be analytical does not have any effect in the proof of RT formula where only analyticity at n = 1 is assumed [15,16].
As mentioned at the beginning, this holographic set-up could provide a simpler and yet rich framework where novel aspects of strongly coupled higher dimensional CFT's could be revealed. It would be interesting to investigate how the inclusion of a U(1) charge in our model would affect the bulk instabilities, and thus the phase transitions in Rényi entropy. A major challenge would be how to holographically realises the non-analytic behaviour of the Rényi entropies found in [77], we leave this for future works.