BPS Black Holes in AdS4 from M-theory

We study supersymmetric black holes in $AdS_4$ in the framework of four dimensional gauged $\N=2$ supergravity coupled to hypermultiplets. We derive the flow equations for a general electrically gauged theory where the gauge group is Abelian and, restricting them to the fixed points, we derive the gauged supergravity analogue of the attractor equations for theories coupled to hypermultiplets. The particular models we analyze are consistent truncations of M-theory on certain Sasaki-Einstein seven-manifolds. We study the space of horizon solutions of the form $AdS_2\times \Sigma_g$ with both electric and magnetic charges and find a four-dimensional solution space when the theory arises from a reduction on $Q^{111}$. For other $SE_7$ reductions, the solutions space is a subspace of this. We construct explicit examples of spherically symmetric black holes numerically.


Introduction
Supersymmetric, asymptotically AdS 4 black holes 1 with regular spherical horizons have recently been discovered in N = 2 gauged supergravities with vector multiplets [1]. These solutions have been further studied in [2,3]. The analytic solution for the entire black hole was constructed and shown to be one quarter-BPS. For particular choices of prepotential and for particular values of the gauge couplings, these black holes can be embedded into M-theory and are asymptotic to AdS 4 × S 7 .
The goal of this work is to study supersymmetric, asymptotically AdS 4 black holes in more general gauged supergravities, with both vector and hypermultiplets. The specific theories we focus on are consistent truncations of string or M-theory. Supersymmetric black holes in these theories involve running hypermultiplet scalars and are substantially different from the examples in [1]. The presence of hypers prevents us from finding analytic solutions of the BPS conditions, nevertheless we study analytically the space of supersymmetric horizon solutions AdS 2 × Σ g and show that there is a large variety of them. We will then find explicit spherically symmetric black hole solutions interpolating between AdS 4 and AdS 2 × S 2 by numerical methods. The black holes we construct have both electric and magnetic charges.
Our demand that the supergravity theory is a consistent truncation of M-theory and that the asymptotic AdS 4 preserves N = 2 supersymmetry limits our search quite severely. Some of the gauged supergravity theories studied in [1] correspond to the N = 2 truncations [4,5] of the de-Wit/Nicolai N = 8 theory [6] where only massless vector multiplets are kept. In this paper we will focus on more general theories obtained as consistent truncations of M-theory on seven-dimensional Sasaki-Einstein manifolds. A consistent truncation of elevendimensional supergravity on a Sasaki-Einstein manifold to a universal sector was obtained in [7,8]. More recently the general reduction of eleven-dimensional supergravity to four dimensions on left-invariant coset manifolds with SU (3)-structure has been performed in [9] 2 . Exploiting the coset structure of the internal manifold it is possible to truncate the theory in such a way to also keep massive Kaluza-Klein multiplets. These reductions can, by their very construction, be lifted directly to the higher dimensional theory and are guaranteed to solve the higher dimensional equations of motion.
The black holes we construct represent the gravitational backreaction of bound states of M2 and M5-branes wrapped on curved manifolds in much the same manner as was detailed by Maldacena and Nunez [20] for D3-branes in AdS 5 × S 5 and M5-branes in AdS 7 × S 4 . To preserve supersymmetry, a certain combination of the gauge connections in the bulk is set equal to the spin connection, having the effect of twisting the worldvolume gauge theory in the manner of [21]. For D3-branes, for particular charges, the bulk system will flow to AdS 3 × Σ g in the IR and the entire solution represents an asymptotically AdS 5 black string. The general regular flow preserves just 2 real supercharges and thus in IIB string theory it is 1 16 -BPS. Similarly, for the asymptotically AdS 7 , black M5-brane solutions, depending on the charges, the IR geometry is AdS 5 × Σ g and the dual CF T 4 may have N = 2 or N = 1 supersymmetry. These N = 2 SCFT's and their generalizations have been of much recent 1 To be precise, the black holes we are discussing will asymptotically approach AdS 4 in the UV but will differ by non-normalizable terms corresponding to some magnetic charge. We will nevertheless refer to them as asymptotically AdS 4 black holes.
By embedding the AdS 4 black holes in M-theory we can see them as M2-brane wrapping a Riemann surface. For particular charges, the bulk system will flow to AdS 2 × Σ g in the IR and represents a black hole with regular horizon. The original examples found in [26] can be reinterpreted in this way; it has four equal magnetic charges and can be embedded in AdS 4 × S 7 . The explicit analytic solution is known and it involves constant scalars and a hyperbolic horizon. A generalization of [20] to M2-branes wrapping Σ g was performed in [27] where certain very symmetric twists were considered. Fully regular solutions for M2 branes wrapping a two-sphere with running scalars were finally found in [1] in the form of AdS 4 black holes. It is note-worthy that of all these scenarios of branes wrapping Riemann surfaces, the complete analytic solution for general charges is known only for M2-branes on Σ g with magnetic charges [1].
One way to generalize these constructions of branes wrapped on Σ g is to have more general transverse spaces. This is the focus of this article. For M5-branes one can orbifold S 4 while for D3-branes one can replace S 5 by an arbitrary SE 5 manifold and indeed a suitable consistent truncation on T 11 has indeed been constructed [18,19]. For M2-branes one can replace S 7 by a seven-dimensional Sasaki-Einstein manifold SE 7 and, as discussed above, the work of [9] provides us with a rich set of consistent truncations to explore. Interestingly, in our analysis we find that there are no solutions for pure M2-brane backgrounds, there must be additional electric and magnetic charges corresponding to wrapped M2 and M5-branes on internal cycles. Asymptotically AdS 4 black holes with more general transverse space can be found in [28] and [29] where the solutions were studied directly in M-theory. These include the M-theory lift of the solutions we give in Sections 4.2.1 and 5.1.
The BPS black holes we construct in this paper are asymptotically AdS 4 and as such they are states in particular (deformed) three-dimensional superconformal field theories on S 2 × R. The solution in [1] can be considered as a state in the twisted ABJM theory [30]. The solutions we have found in this paper can be seen as states in (twisted and deformed) three dimensional Chern-Simons matter theory dual to the M-theory compactifications of homogeneous Sasaki-Einstein manifolds 3 . One feature of these theories compared to ABJM is the presence of many baryonic symmetries that couple to the vector multiplets arising from non trivial two-cycles in the Sasaki-Einstein manifold. In terms of the worldvolume theory, the black holes considered in this paper are then electrically charged states of a Chern-Simons matter theory in a monopole background for U (1) R symmetry and other global symmetries, including the baryonic ones 4 .
Gauged N = 2 supergravity with hypermultiplets is the generic low-energy theory arising from a Kaluza-Klein reduction of string/M-theory on a flux background. The hyper-multiplet scalars interact with the vector-multiplet scalars through the scalar potential: around a generic AdS 4 vacuum the eigenmodes mix the hypers and vectors. In the models we study, we employ a particular simplification on the hypermultiplet scalar manifold (2.7) and find solutions where only one real hypermultiplet scalar has a non-trivial profile. Given that the simplification is so severe it is quite a triumph that solutions exist within this ansatz. It would be interesting to understand if this represents a general feature of black holes in gauged supergravity.
The paper is organized as follows. In Section 2 we summarize the ansatz we use and the resulting BPS equations for an arbitrary electrically gauged N = 2 supergravity theory. The restriction of the flow equations to the horizon produces gauged supergravity analogues of the attractor equations.
In Section 3 we describe the explicit supergravity models we consider. A key step is that we use a symplectic rotation to a frame where the gauging parameters are purely electric so that we can use the supersymmetry variations at our disposal.
In Section 4 we study horizon geometries of the form AdS 2 × Σ g where g = 1. We find a four parameter solution space for Q 111 and the solutions spaces for all the other models are truncations of this space.
In Section 5 we construct numerically black hole solutions for Q 111 and for M 111 . The former solution is a gauged supergravity reproduction of the solution found in [29] and is distinguished in the space of all solutions by certain simplifications. For this solution, the phase of the four dimensional spinor is constant and in addition the massive vector field vanishes. The solution which we construct in M 111 turns out to be considerably more involved to compute numerically and has all fields of the theory running. In this sense we believe it to be representative of the full solution space in Q 111 .

The Black Hole Ansatz
We want to study static supersymmetric asymptotically AdS 4 black holes in four-dimensional N = 2 gauge supergravity. The standard conventions and notations for N = 2 gauge supergravity [40,41] are briefly reviewed in Appendix A.
Being supersymmetric, these black holes can be found by solving the supersymmetry variations (A.16) -(A.18) plus Maxwell equations (A.14). In this section we give the ansatz for the metric and the gauge fields, and a simplified form of the SUSY variations we will study in the rest of this paper. The complete SUSY variations are derived and discussed in Appendix B.

The Ansatz
We will focus on asymptotically AdS 4 black holes with spherical (AdS 2 × S 2 ) or hyperbolic (AdS 2 × H 2 ) horizons. The modifications required to study AdS 2 × Σ g horizons, where Σ g is a Riemann surface of genus g, are discussed at the end of Section 2.2. The ansatz for the metric and gauge fields is 3) The electric and magnetic charges are where G Λ is the symplectic-dual gauge field strength In addition, we assume that all scalars in the theory, the fields z i from the n v -vector multiplets and q u from the n h -hypermultiplets, are functions of the radial co-ordinate r, only. Moreover, we will restrict our analysis to abelian gaugings of the hypermultiplet moduli space and assume that the gauging is purely electric. As discussed in [42], for Abelian gauge groups one can always find a symplectic frame where this is true.

The BPS Flow Equations
In Appendix B, we derive the general form that the SUSY conditions take with our ansatz for the metric and gauge fields and the hypothesis discuss above for the gaugings. We will only consider spherical and hyperbolic horizons.
Throughout the text, when looking for explicit black hole solutions we make one simplifying assumption, namely that the Killing prepotentials P x Λ of the hypermultiplet scalar manifold M h satisfy 5 The flow equations given in this section reduce to the equations in [2,3] when the hypermultiplets are truncated away and thus P 3 Λ are constant.

The preserved supersymmetry is
where 0A is an SU (2)-doublet of constant spinors which satisfy the following projections As a result only 2 of the 8 supersymmetries are preserved along any given flow. Imposing these two projections, the remaining content of the supersymmetry equations reduces to a set of bosonic BPS equations. Some are algebraic and some differential where we have absorbed a phase in the definition of the symplectic sections Z denotes the central charge Once P 3 Λ are fixed, the ±-sign in the equations above can be absorbed by a redefinition (p Λ , q Λ , e U ) → −(p Λ , q Λ , e U ).
Since the gravitino and hypermultiplets are charged, there are standard Dirac quantization conditions We see from (2.11) and (2.12) that the BPS conditions select a particular integer quantization.

Maxwell's equation becomes
Notice that for the truncations of M-theory studied in this work, the non-trivial RHS will play a crucial role since massive vector fields do not carry conserved charges.
Using standard special geometry relations, one can show that the variation for the vector multiplet scalars and the warp factor U , (2.16) and (2.18), are equivalent to a pair of constraints for the sections L Λ Importantly we can integrate (2.28) to get for some constant c Λ . From (2.14) and (2.15) we see that this gauge invariance is constrained to satisfy c Λ P 3 We note that due to the constraint on the sections (2.28) and (2.29) give (2n v + 1)-equations.
One can show that the algebraic relation (2.13) is an integral of motion for the rest of the system. Specifically, differentiating (2.13) one finds a combination of the BPS equations plus Maxwell equations contracted with L Λ i . One can solve (2.13) for ψ and find that it is the phase of a modified "central charge" Z: Our analysis also applies to black holes with AdS 2 × Σ g horizons, where Σ g is a Riemann surface of genus g ≥ 0. The case g > 1 is trivially obtained by taking a quotient of H 2 by a discrete group, since all Riemann surfaces with g > 1 can be obtained in this way. Our system of BPS equations (2.11) -(2.20) also applies to the case of flat or toroidal horizons (g = 1) provided we substitute the constraint (2.11) with We will not consider explicitly the case of flat horizons in this paper although they have attracted some recent interest [29].

AdS 2 × S 2 and AdS 2 × H 2 Fixed Point Equations
At the horizon the scalars (z i , q u ) are constant, while the functions in the metric and gauge fields take the form with q Λ 0 constant. The BPS equations are of course much simpler, in particular they are all algebraic and there are additional superconformal symmetries.
There are the two Dirac quantization conditions The radii are given by (2.16) and (2.17) In addition, the algebraic constraint (2.13) becomes Im (e −iψ Z) = 0 (2.46) and the hyperino variation gives Finally, combining (2.30), (2.29) and (2.5), we can express the charges in terms of the scalar fields with M i Λ = Im (e −iψ M Λ ). These are the gauged supergravity analogue of the attractor equations.
It is of interest to solve explicitly for the spectrum of horizon geometries in any given gauged supergravity theory. In particular this should involve inverting (2.48) and (2.49) to express the scalar fields in terms of the charges. Even in the ungauged case, this is in general not possible analytically and the equations here are considerably more complicated. Nonetheless one can determine the dimension of the solution space and, for any particular set of charges, one can numerically solve the horizon equations to determine the value of the various scalars. In this way one can check regularity of the solutions.

Consistent Truncations of M-theory
Having massaged the BPS equations into a neat set of bosonic equations we now turn to particular gauged supergravity theories in order to analyze the space of black hole solutions. We want to study models which have consistent lifts to M-theory and which have an N = 2 AdS 4 vacuum somewhere in their field space, this limits our search quite severely. Two examples known to us are N = 2 truncations of the de-Wit/Nicolai N = 8 theory [6] and the truncation of M-theory on SU (3)-structure cosets [9]. In this paper we will concentrate on some of the models constructed in [9]. The ones of interest for us are listed in Table 1. Table 1: The consistent truncations on SU (3)-structure cosets being considered in this work. M 7 is the 7-manifold, the second column is the number of massless vector multiplets at the AdS 4 vacuum, the third column is the number of massive vector multiplets and final column is the number of hypermultiplets.
For each of these models there exists a consistent truncation to an N = 2 gauge supergravity with n v vector multiplets and n h hypermultiplets. We summarize here some of the features of these models referring to [9] for a more detailed discussion.
We denote the vector multiplets scalars where the number of vector multiplets n v can vary from 0 to 3. Notice that all models contain some massive vector multiplets. For the hypermultiplets, we use the notation where a, φ belong to the universal hypermultiplet. This is motivated by the structure of the quaternionic moduli spaces in these models, which can be seen as images of the c-map. The metric on quaternionic Kähler manifolds of this kind can be written in the form [43] where {z i , z  |i = 1, . . . , n h − 1} are special co-ordinates on the special Kähler manifold M c and {ξ A ,ξ A |A = 1, . . . , n h } form the symplectic vector ξ T = (ξ A ,ξ A ) and are co-ordinates on the axionic fibers.
All these models, and more generally of N = 2 actions obtained from compactifications, have a cubic prepotential for the vector multiplet scalars and both magnetic and electric gaugings of abelian isometries of the hypermultiplet scalar manifold. In ungauged supergravity the vector multiplet sector is invariant under Sp(2n v + 2, R). The gauging typically breaks this invariance, and we can use such an action to find a symplectic frame where the gauging is purely electric 6 . Since Sp(2n v + 2, R) acts non trivially on the prepotential F, the rotated models we study will have a different prepotential than the original ones in [9] .

The Gaugings
In the models we consider, the symmetries of the hypermultiplet moduli space that are gauged are non compact shifts of the axionic fibers ξ A and U (1) rotations of the special Kähler basis z i . The corresponding Killing vectors are the Heisenberg vector fields: For some purposes it is convenient to work in homogeneous co-ordinates on M c where U is a 2n h × 2n h matrix of gauging parameters. In special co-ordinates k U is a sum of the Killing vectors f A and g.
A general electric Killing vector field of the quaternionic Kähler manifold is given by where Q ΛA and Q A Λ are also matrices of gauge parameters, while the magnetic gaugings are parameterized by [9] For these models, the resulting Killing prepotentials can be worked out using the property where ω x u is the spin connection on the quaternionic Kähler manifold [43] The Killing vector k U may contribute a constant shift to P 3 0 , and this is indeed the case for the examples below.
As already mentioned, we will work in a rotated frame where all gaugings are electric. The form of the Killing vectors and prepotentials is the same, with the only difference that nowk Λ = −m Λ h andP x Λ will add an extra contribution to the electric ones.

The Models
The models which we will study are summarized in Table 1. They all contain an AdS 4 vacuum with N = 2 supersymmetry. The vacuum corresponds to the ansatz (2.1) with warp factors (3.14) and no electric and magnetic charges The AdS 4 radius and the non trivial scalar fields are This is not an exact solution of the flow equations in Section 2.2 which require a non-zero magnetic charge to satisfy (2.11). The black holes of this paper will asymptotically approach AdS 4 in the UV but will differ by non-normalizable terms corresponding to the magnetic charge. The corresponding asymptotic behavior has been dubbed magnetic AdS in [44].

Q 111
The scalar manifolds for the Q 111 truncation are .
The metric on M 2,1 is 18) and the special Kähler base M c is trivial. Nonetheless we can formally use the prepotential and special co-ordinates on M c to construct the spin connection and Killing prepotentials.
The natural duality frame which arises upon reduction has a cubic prepotential 7 with sections X Λ = (1, z ) and both electric and magnetic gaugings Using an element S 0 ∈ Sp(8, Z) we rotate to a frame where the gaugings are purely electric. Explicitly we have and the new gaugings are The Freund-Rubin parameter e 0 > 0 is unfixed. In this duality frame the special geometry data are (3.26)

M 111
The consistent truncation on M 111 has and is obtained from the Q 111 reduction by truncating a single massless vector multiplet. This amounts to setting The consistent truncation of M-theory on N 11 has one massless and two massive vector multiplets, along with two hypermultiplets. The scalar manifolds are .
The metric on M 2,4 is 30) and the special co-ordinate z on the base is given by (3.31) This differs slightly from the special co-ordinate used in [9], where the metric is taken on the upper half plane instead of the disk. The prepotential and special co-ordinates on M c are given by The cubic prepotential on M v obtained from dimensional reduction is the same as for Q 111 , (3.20), however the models differ because of additional gaugings The duality rotation we used for the Q 111 model to make the gaugings electric would not work here since it would then make (3.33) magnetic. However using the fact that m Λ and we can find a duality frame where all parameters are electric and Q A Λ is unchanged. Explicitly we use The Killing vectors are then given by (3.23) and (3.33). The prepotential in this frame is rather complicated in terms of the new sections, which are in turn given as a function of the scalar fields z i by (2) Sp (1) This is obtained from the N 11 model by eliminating the massless vector multiplet. Explicitly, this is done by setting In addition to the N = 2, round S 7 solution (3.16) this model contains in its field space the squashed S 7 solution, although this vacuum has only N = 1 supersymmetry. Thus flows from this solution lie outside the ansatz employed in this work.
3.2.5 Universal SU (4) SU (3) Truncation This model was first considered in [8]. It contains just one massive vector multiplet and one hyper multiplet, and can be obtained from the M 111 truncation by setting (3.41)

Horizon Geometries
We now apply the horizon equations of Section 2.3 to the models of Section 3. We find that there is a four dimensional solution space within the Q 111 model and that this governs all the other models, even though not all the other models are truncations of Q 111 . The reason is that the extra gaugings present in the N 11 and squashed S 7 model can be reinterpreted as simple algebraic constraints on our Q 111 solution space.
In the following, we will use the minus sign in (2.11) and subsequent equations. We also recall that κ = 1 refers to AdS 2 × S 2 and κ = −1 to AdS 2 × H 2 horizons.

M-theory Interpretation
The charges of the four-dimensional supergravity theory have a clear interpretation in the eleven-dimensional theory. This interpretation is different from how the charges lift in the theory used in [1], which we now review. In the consistent truncation of M-theory on S 7 [45,46] the SO(8)-vector fields lift to Kaluza-Klein metric modes in eleven-dimensions. In the further truncation of [4,5] only the four-dimensional Cartan subgroup of SO(8) is retained, the magnetic charges of the four vector fields in [1] lift to the Chern numbers of four U (1)bundles over Σ g . One can interpret the resulting AdS 4 black holes as the near horizon limit of a stack of M2-branes wrapping Σ g ⊂ X 5 , where X 5 is a praticular non-compact Calabi-Yau five-manifold, constructed as four line bundles over Σ g : A similar description holds for wrapped D3-branes and wrapped M5-branes in the spirit of [20]. The general magnetic charge configurations have been analyzed recently for D3 branes in [47] and M5-branes in [25]. Both these works have computed the field theory central charge and matched the gravitational calculation 8 . This alone provides convincing evidence that the holographic dictionary works for general twists. There has not yet been any such computation performed from the quantum mechanics dual to the solutions of [1], but, as long as the charges are subject to appropriate quantization so as to make X 5 well defined, one might imagine there exist well defined quantum mechanical duals of these solutions. Now returning to the case at hand, the eleven-dimensional metric from which the fourdimensional theory is obtained is [9] ds 2 11 = e 2V K −1 ds 2 4 + e −V ds 2 where B 6 is a Kähler-Einstein six-manifold, θ is the Sasaki fiber, V is a certain combination of scalar fields (not to be confused with V in (2.1)), K = 1 8 e −K with K the Kähler potential, and A 0 is the four-dimensional graviphoton 9 . In addition, vector fields of massless vector multiplets come from the three-form potential expanded in terms of cohomologically nontrivial two forms ω i The truncations discussed above come from reductions with additional, cohomologically trivial two-forms, which give rise to the vector fields of massive vector mutliplets. This is an important issue for our black hole solutions since only massless vector fields carry conserved charges.
The solutions described in this section carry both electric and magnetic charges. The graviphoton will have magnetic charge p 0 given by (4.15), which means the eleven-dimensional geometry is really of the form where M 9 is a nine-manifold which can be described as a U (1) fibration The electric potential q 0 will vanish from which we learn that this U (1) is not fibered over AdS 2 , or in other words the M2 branes that wrap Σ g do not have momentum along this U (1).
In addition the charges that lift to G (4) correspond to the backreaction of wrapped M2 and M5-branes on H 2 (SE 7 , Z) and H 5 (SE 7 , Z). We can check that the Chern number of this U (1) fibration is quantized as follows. First we have θ + where ψ has periodicity 2π for some ∈ R and η is a Kähler potential one-form on B 6 which satisfies dη = 2J. Such a fibration over a sphere is well defined if Recalling (2.4) and preempting (4.15), we see that For the SE 7 admitting spherical horizons used in this paper one has and (4.7) is satisfied. 9 There is a factor of √ 2 between A Λ here and in [9], see footnote 10 of that paper.

Q 111
To describe the solution space of AdS 2 × S 2 or AdS 2 × H 2 solutions, we will exploit the fact that the gaugings (3.21) are symmetric in the indices i = 1, 2, 3. We can therefore express the solution in terms of invariant polynomials under the diagonal action of the symmetric group S 3 First we enforce (2.7), which gives The Killing prepotentials are then given by Solving (2.40) and (2.41) we get two constraints on the magnetic charges We find that the phase of the spinor is fixed Then from (2.47) we get We can of course break the symmetry and solve the equations above for, for instance, (4.20) Using (2.44) we find the radius of AdS 2 to be The algebraic constraint (2.13) is nontrivial and can be used to solve for q 0 in terms of (p Λ , q i , v j , b k ). 10 For example σ(v 2 Using the value of p 0 given in (4.15) we can solve (2.48) and (2.49) and find , (4.22) where The charges (p 2 , p 2 , q 2 , q 3 ) are related to (p 1 , q 1 ) by symmetry of the i = 1, 2, 3 indices. The general solution space has been parameterized by (v i , b j ) subject to the two constraints (4.17) and (4.18) leaving a four dimensional space. From these formula, one can easily establish numerically regions where the horizon geometry is regular. A key step omitted here is to invert these formulae and express the scalars (b i , v j ) in terms of the charges (p Λ , q Λ ). This would allow one to express the entropy and the effective AdS 2 radius in term of the charges [50].

A Q 111 simplification
The space of solutions in the Q 111 model simplifies considerably if one enforces a certain symmetry p 1 = p 2 , q 1 = −q 2 . (4.31) One then finds a two-dimensional space of solutions part of which was found in [28,29] where 1 = ± is a choice. One cannot analytically invert (4.38) and (4.41) to give (v 1 , v 3 ) in terms of (p 1 , q 1 ) but one can numerically map the space of charges for which regular solutions exist.

M 111
The truncation to the M 111 model (3.28) does not respect the simplification (4.31). The general solution space is two-dimensional , (4.47) , (4.48) (4.52) where 2 is a choice of sign.

N 11
In setting P 1 Λ = P 2 Λ = 0 we get  From this one can deduce that the spectrum of horizon solutions will be obtained from that of Q 111 by imposing two additional constraints which amount to One can then deduce that the AdS 2 × Σ g solution space in the N 11 model is a twodimensional restriction of the four dimensional space from the Q 111 model. While (4.62) can easily be performed on the general solution space, it is somewhat more difficult to enforce (4.61) since the charges are given in terms of the scalars. We can display explicitly a onedimensional subspace of the N 11 family by further setting v 3 = v 1 : , (4.69) , (4.70) 3)e 2 0 + 9(11 , (4.72) , (4.73) , (4.74) . (4.75)

Sp(2)
Sp (1) The truncation of M-theory on Sp(2) Sp(1) is obtained from the N 11 truncation by removing a massless vector multiplet. Explcitly, this is done by setting

SU (3)
This solution is unique and requires κ = −1. Therefore it only exists for hyperbolic horizons: It is connected to the central AdS 4 vacuum by a flow with constant scalars, which is known analytically [26] .

Black Hole solutions: numerical analysis
Spherically symmetric, asymptotically AdS static black holes can be seen as solutions interpolating between AdS 4 and AdS 2 × S 2 . We have seen that AdS 2 × S 2 vacua are quite generic in the consistent truncations of M-theory on Sasaki-Einstein spaces and we may expect that they arise as horizons of static black holes. In this section we will show that this is the case in various examples and we expect that this is true in general.
The system of BPS equations (2.11) -(2.20) can be consistently truncated to the locus this condition is satisfied at the fixed points and enforces (2.7) along the flow. The only running hyperscalar is the dilaton φ. The solutions of (2.11) -(2.20) will have a non trivial profile for the dilaton, all the scalar fields in the vector multiplets, the gauge fields and the phase of the spinor. This makes it hard to solve the equations analytically. We will find asymptotic solutions near AdS 4 and AdS 2 × S 2 by expanding the equations in series and will find an interpolating solution numerically. The problem simplifies when symmetries allow to set all the massive gauge fields and the phase of the spinor to zero. A solution of this form can be found in the model corresponding to the truncation on Q 111 . The corresponding solution is discussed in Section 5.1 and it corresponds to the class of solutions found in eleven dimensions in [29]. The general case is more complicated. The M 111 solution discussed in Section 5.2 is an example of the general case, with most of the fields turned on.

Black Hole solutions in Q 111
We now construct a black hole interpolating between the AdS 4 ×Q 111 vacuum and the horizon solutions discussed in Section 4.2.1 with The solution should correspond to the M-theory one found in [29]. Due to the high degree of symmetry of the model, we can truncate the set of fields appearing in the solution and consistently set along the flow. This restriction is compatible with the following simplification on the gauge fieldsq 2 (r) = −q 1 (r) ,q 0 (r) = 0 ,q 3 (r) = 0 . For simplicity, we study the interpolating solution corresponding to the horizon solution in Section 4.2.1 with v 1 = v 3 . This restriction leaves a family of AdS 2 × S 2 solutions which can be parameterized by the value of v 1 or, equivalently, by the magnetic charge p 1 . We perform our numerical analysis for the model with and electric and magnetic charges We fixed e 0 = 8 √ 2. The values of the scalar fields at the AdS 4 point are given in (3.16).
It is convenient to define a new radial coordinate by dt = e −U dr. t runs from +∞ at the AdS 4 vacuum to −∞ at the horizon. It is also convenient to re-define some of the scalar such that they vanish at the AdS 4 point. The metric functions will be also re-defined This set of equations has two obvious symmetries. Given a solution, we can generate other ones by 12) or by translating all fields φ i in the solution where d 1 and d 2 are arbitrary constants.
We can expand the equations near the AdS 4 UV point. We should stress again that AdS 4 is not strictly a solution due to the presence of a magnetic charge at infinity. However, the metric functions u and v approach the AdS 4 value and, for large t, the linearized equations of motion for the scalar fields are not affected by the magnetic charge, so that we can use much of the intuition from the AdS/CFT correspondence. The spectrum of the consistent truncation around the AdS 4 vacuum in absence of charges have been analyzed in details in [9]. It consists of two massless and one massive vector multiplet (see Table 1). By expanding the BPS equations for large t we find that there exists a family of asymptotically (magnetic) AdS solutions depending on three parameters, corresponding to two operators of dimension ∆ = 1 and an operator of dimension ∆ = 4. The asymptotic expansion of the solution is (5.14) where the dots refer to exponentially suppressed terms in the expansion in e −t or to terms at least quadratic in the parameters ( 1 , 4 , β 1 ). We also set two arbitrary constant terms appearing in the expansion of u(t) and v(t) to zero for notational simplicity; they can be restored by applying the transformations (5.12) and (5.13). The constants 1 and β 1 correspond to scalar modes of dimension ∆ = 1 in the two different massless vector multiplets (cfr Table 7 of [9]). The constant 4 corresponds to a scalar mode with ∆ = 4 belonging to the massive vector multiplet. A term te −4t shows up at the same order as 4 and it is required for consistency. Notice that, although e 1 = e 3 both at the UV and IR, the mode e 1 − e 3 must be turned on along the flow. In the IR, AdS 2 × S 2 is an exact solution of the BPS system. The relation between the two radial coordinates is r − r 0 ∼ e at with a = 8 2 1/4 /3 1/4 , where r 0 is the position of the horizon. By linearizing the BPS equations around AdS 2 × S 2 we find three normalizable modes with behavior e a∆t with ∆ = 0, ∆ = 1 and ∆ = 1.37. The IR expansion is obtained as a double series in e at and e where the numbers d p,q can be determined numerically at any given order. The two symmetries (5.12) and (5.13) are manifest in this expression and correspond to combinations of a shift in c 1 and suitable rescalings of c 2 and c 3 . With a total number of six parameters for six equations we expect that the given IR and UV expansions can be matched at some point in the middle, since the equations are first order and the number of fields is equal to the number of parameters. There will be precisely one solution with the UV and IR asymptotics given above; the general solution will be obtained by applying the transformations (5.12) and (5.13). We have numerically solved the system of BPS equation and tuned the parameters in order to find an interpolating solution. The result is shown in Figure 1. We would like to stress that the asymptotic expansions of the solutions contain integer powers of r (and logs) in the UV (AdS 4 ) and irrational powers depending on the charges in the IR (AdS 2 × S 2 ). This suggests that it would be hard to find analytic solutions of the system of BPS equations (2.11) -(2.20) with running hypermultiplets. By contrast, the static AdS 4 black holes in theories without hypermultiplets [1] depends only on rational functions of r which made it possible to find an explicit analytic solution.

Black Hole solutions in M 111
Whenever we cannot enforce any symmetry on the flow, things are much harder. This is the case of the interpolating solutions for M 111 which we now discuss. The solution can be also embedded in the Q 111 model and it is a general prototype of the generic interpolating solution between AdS 4 and the horizons solutions discussed in Section 4.
Let us consider an interpolating solution corresponding to the horizon discussed in Section 4.3. The conditions (5.5) cannot be imposed along the flow. As a consequence, the phase of the spinor will run and a massive gauge field will be turned on. Moreover, the IR conditions b 2 = −2b 1 andq 0 =q 3 = 0,q 2 = −q 1 do not hold for finite r and all gauge and vector scalar fields are turned on. The only simplification comes from the fact that on the locus (5.1) the right hand side of Maxwell equations (2.27) is proportional to k a Λ . For M 111 , k a 1 = k a 2 and we still have two conserved electric charges In other words, two Maxwell equations can be reduced to first order constraints while the third remains second order. It is convenient to transform the latter equation into a pair of first order constraints. This can be done by introducing q 0 as a new independent field and by using one component of Maxwell equations and the definition (2.5) of q Λ as a set of four first order equations for (q 0 ,q 1 ,q 2 , q 0 ). The set of BPS and Maxwell equations consists of twelve first order equations for twelve variables A major simplification arises if we integrate out the gauge fields using (2.30). The system collapses to a set of eight first order equations for eight unknowns. The resulting set of equations have singular denominators and it is convenient to keep the extra field q 0 and study a system of nine first order equations for 18) The final system has an integral of motion which would allow to eliminate algebraically q 0 in terms of the other fields.
The system of BPS equations is too long to be reported here but it can be studied numerically and by power series near the UV and the IR. We will study the flow to the one-parameter family of horizon solutions with v 1 = v 2 and b 2 = −2b 1 . These horizons can be parametrized by the value of v 1 or, equivalently, by the magnetic charge p 2 . We perform our numerical analysis for the model with and electric and magnetic charges We fixed e 0 = 24 √ 2. The values of the scalar fields at the AdS 4 point are given in (3.16). As in the previous section, it is also convenient to define a new radial coordinate by dt = e −U dr and to re-define some of the scalar fields and metric functions In absence of charges, the spectrum of the consistent truncation around the AdS 4 vacuum consists of one massless and one massive vector multiplet [9] (see Table 1). By expanding the BPS equations for large t we find that there exists a family of asymptotically (magnetic) AdS solutions depending on three parameters corresponding to operators of dimension ∆ = 1, ∆ = 4 and ∆ = 5. The asymptotic expansion of the solution is where the dots refer to exponentially suppressed terms in the expansion in e −t or to terms at least quadratic in the parameters ( 1 , ρ 4 , β 1 , m 3 ). As for the Q 111 black hole, we set two arbitrary constant terms in the expansion of u(t) and v(t) to zero for notational simplicity; they can be restored applying the transformations (5.12) and (5.13). The parameters 1 and β 1 are associated with two modes with ∆ = 1 belonging to the massless vector multiplet, while the parameters ρ 4 and m 3 correspond to a scalar with ∆ = 4 and a gauge mode with ∆ = 5 in the massive vector multiplet (cfr Table 7  The mode with ∆ = 0 is just a common shift in the metric functions corresponding to the symmetry (5.12). The other modes give rise to a triple expansion in powers p,q,r d p,q,r c p 1 c q 2 c r 3 e (p+1.44q+1.58r)at (5.23) of all the fields. We have a total number of eight parameters for nine equations which possess an algebraic integral of motion. We thus expect that the given IR and UV expansions can be matched at finite t. With some pain and using a precision much greater than the one given in the text above, we have numerically solved the system of BPS equation and found an interpolating solution. The result is shown in Figure 2.

A Four Dimensional Gauged Supergravity
In this Appendix, in order to fix notation and conventions, we recall few basic facts about N = 2 gauge supergravity. We use the standard conventions of [40,41].
The scalars in the vector multiplets parametrise a special Kähler manifold of complex dimension n V , M SK , with metric where K(z,z) is the Kähler potential on M SK . This can be computed introducing homogeneous coordinates X Λ (z) and define a holomorphic prepotential F(X), which is a homogeneous function of degree two where F Λ = ∂ Λ F . In the paper we will use both the holomorphic sections (X Λ , F Λ ) and the symplectic sections The scalars in the hypermultiplets parametrise a quaternionic manifold of real dimension 4n H , M Q , with metric h uv .
The bosonic Lagrangian is where Λ, Σ = 0, 1, . . . , n V . The gauge field strengths are defined as . In this notation, A 0 is the graviphoton and A Λ , with Λ = 1, . . . , n V , denote the vectors in the vector multiplets. The matrix N ΛΣ of the gauge kinetic term is a function of the vector multiplet scalars The covariant derivatives are defined as where k i Λ and k u Λ are the Killing vectors associated to the isometries of the vector and hypermultiplet scalar manifold that have been gauged. In this paper we will only gauge (electrically) abelian isometries of the hypermultiplet moduli space. The Killing vectors corresponding to quaternionic isometries have associated prepotentials: these are a set of real functions in the adoint of SU(2), satisfying where Ω x uv = dω x + 1/2 xyz ω y ∧ ω z and ∇ v are the curvature and covariant derivative on M Q . In the specific models we consider in the text, one can show that the Killing vectors preserve the connection ω x and the curvature Ω x uv . This allows to simplify the prepotential equations, which reduce to Typically in models obtained from M /string theory compactifications, the scalar fields have both electric and magnetic charges under the gauge symmetries. However, by a symplectic transformation of the sections (X Λ , F Λ ), it is always possible to put the theory in a frame where all scalars are electrically charged. Such a transformation 11 leaves the Kähler potential invariant, but changes the period matrix and the preprepotential F(X) .
The models we consider in this paper [9] are of this type: they have a cubic prepotential and both electrical and magnetic gaugings of some isometries of the hypermultiplet moduli space. The idea is then to perform a sympletic rotation to a frame with purely electric gaungings, allowing for sections ( X Λ , F Λ ) which are a general symplectic rotation of those obtained from the cubic prepotential.
The scalar potential in (A.4) couples the hyper and vector multiplets, and is given by where L Λ are the symplectic sections on M SK , f Λ i = (∂ i + 1 2 ∂ i K)L Λ and P x Λ are the Killing prepotentials.
Maxwell's equation is where, for simplicity of notation, we have defined the following matrices acts on the period matrix N ΛΣ by a fractional transformation The full Lagrangian is invariant under N = 2 supersymmetry. In the electric frame, the variations of the fermionic fields are given by where U Bβ u are the vielbeine on the quaternionic manifold and Notice that the covariant derivative on the spinors contains a contribution from the gauge fields from the vector-U (1) connection the hyper-SU (2) connection and the gaugings (see eqs. 4.13,7.57, 8.5 in [41])

B Derivation of the BPS Equations
In this section we consider an ansatz for the metric and the gauge fields that allows for black-holes with spherical or hyperbolic horizons, and we derive the general conditions for 1/4 BPS solutions. The metric and the gauge fields are taken to be where the warp factors U and V are functions of the radial coordinate r and The modifications needed for the flat case are discussed at the end of Section 2.2.
We also assume that all scalars in the vector and hypermultiplets, as well as the Killing spinors A are functions of the radial coordinate only.
To derive the BPS conditions it is useful to introduce the central charge where q Λ is defined in (2.5) and its covariant derivative In the case of flat space we need to replace κp Λ → −p Λ in the definition (2.5) of q Λ and in the above expression for Z.

B.1 Gravitino Variation
With the ansatz (B.1), the gravitino variations (A.16) become where, to simplify notations, we introduced the quantity M ± = γ 01 Z ± iγ 02 (F −1 F I ΛΣ L Λ p Σ ) . (B.10) Let us consider first (B.6). The term proportional to F must be separately zero, since it is the only θ-dependent one. This implies I ΛΣ L Λ p Σ = 0 . (B.11) Similarly, setting to zero the θ-dependent terms in (B.9), which is the usual statement of setting the gauge connection equal to the spin connection, gives the projector This constraint also holds in the case of flat horizon if we set κ = 0. The θ-independent parts of (B.9) and (B.8) are equal and give a second projector Subtracting the θ independent parts of (B.6) and (B.8) gives a third projector (B.14) Finally, subtracting (B.7) and (B.6) we obtain an equation for the radial dependence of the spinor In total we get three projectors, (B.12) -(B.14), one differential relation on the spinor (B.15) and one algebraic constraint (B.11). The idea is to further simply these equations so as to ensure that we end up with two projectors. From now on we will specify to the case of spherical or hyperbolic symmetry, since this is what we will use in the paper. In order to reduce the number of projectors we impose the constraint q Λ P x Λ = c e 2U p Λ P x Λ , x = 1, 2, 3 (B. 16) for some real function c. By squaring (B.12) we obtain the algebraic condition which can be used to rewrite (B.16) as Substituting (B.12) in (B.14) and using (B.18), we obtain the projector which, squared, gives the norm of Z Using the projectors above, (B.15) becomes

B.2 Gaugino Variation
The gaugino variation is M is the only θ-dependent term and must be set to zero separately, giving

B.3 Hyperino Variation
The hyperino variation gives First off, we need to set the θ-dependent part to zero The projectors (B.12) and (B.21) can be used to simply the remaining equation which can then be reduced to a scalar equation Using the standard relations (we use the conventions of [40]) we can reduce (B.35) to The real and imaginary parts givė (B.39)

B.4 Summary of BPS Flow Equations
It is worthwhile at this point to summarize the BPS equations. The algebraic equations are while the differential equations are In the case of flat horizon equation (B.41) is replaced by (p Λ P x Λ ) 2 = 0.

B.5 Maxwell's Equation
Maxwell's equation is In the case of flat horizon we need to replace κp Λ → −p Λ .