Supersymmetric AdS6 black holes from F(4) gauged supergravity

In F (4) gauged supergravity in six dimensions, we study supersymmetric AdS6 black holes with various horizon geometries. We find a new AdS2×Σg1×Σg2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ Ad{S}_2 \times {\Sigma}_{\mathfrak{g}1}\times {\Sigma}_{\mathfrak{g}2} $$\end{document} horizon solution with g1>1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ {\mathfrak{g}}_1>1 $$\end{document} and g2>1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ {\mathfrak{g}}_2>1 $$\end{document}, and present the black hole solution numerically. The full black hole is an interpolating geometry between the asymptotically AdS6 boundary and the AdS2×Σg1×Σg2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ Ad{S}_2 \times {\Sigma}_{\mathfrak{g}1}\times {\Sigma}_{\mathfrak{g}2} $$\end{document} horizon. We calculate the Bekenstein-Hawking entropy of the black hole and find a match with the recently calculated topologically twisted index of 5d USp(2N) gauge theory on Σg1×Σg2×S1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ {\Sigma}_{\mathfrak{g}1}\times {\Sigma}_{\mathfrak{g}2}\times {S}^1 $$\end{document} in the large N limit. We also find black hole horizons of Kähler four-cycles in Calabi-Yau fourfolds and on Cayley four-cycles in Spin(7) manifolds.


Introduction
The AdS 6 /CFT 5 correspondence remains as one of the less appreciated among its family [1]. In SU(2) × U (1)-gauged N = 4 supergravity in six dimensions, commonly known as F (4) gauged supergravity named after the F (4) superalgebra in six dimensions, there is a unique supersymmetric fixed point [2]. This fixed point is known to be dual of 5d superconformal USp(2N ) gauge theory [3] which is one of the few 5d SCFTs known so far [4,5]. In [6] it was shown that F (4) gauged supergravity is a consistent truncation of massive type IIA supergravity [7]. 1 The fixed point uplifts to AdS 6 × S 4 near-horizon geometry of the D4-D8 brane system [8].
In order to study RG flows from 5d SCFTs to lower dimensional ones via the AdS/CFT correspondence in the spirit of [12], twisted compactifications of F (4) gauged supergravity were studied. The supergravity solutions describe the near-horizon geometries of wrapped D4-branes on various supersymmetric cycles. D4-branes wrapped on two-and three-cycles were studied in [13,14]. They found AdS 4 and AdS 3 fixed point solutions. See for more recent results on three-cycles in [15].
In this paper, we study supersymmetric AdS 6 black hole solutions by considering D4-branes wrapped on supersymmetric four-cycles. We begin by deriving supersymmetry equations for D4-branes wrapped on two Riemann surfaces and find a new AdS 2 × H 2 × H 2 solution. When we consider S 2 × S 2 background, there is no AdS 2 fixed point. We also JHEP01(2019)035 present the full black hole solution numerically, which is an interpolating geometry between the asymptotically AdS 6 boundary and the AdS 2 × H 2 × H 2 horizon. We calculate entropy of asymptotically AdS 6 black holes with AdS 2 ×Σ g 1 ×Σ g 2 horizon where g 1 > 1 and g 2 > 1. Here Σ g is a Riemann surface of genus g with constant curvature. Analogous to the 3d gauge theory examples in [16][17][18], this entropy would give the topologically twisted index of 5d USp(2N ) gauge theory on Σ g 1 × Σ g 2 × S 1 in the large N limit. Indeed we find that the entropy nicely matches the recent calculation of topologically twisted index in [19].
In contrast to the black hole solutions which exist only for g 1 > 1 and g 2 > 1, topologically twisted index is well defined for arbitrary genus. When a black hole solution exists, the index is counting the entropy of the black hole, however, the inverse is not true, i.e. even if the index is well defined, it does not guarantee that there is a corresponding black hole solution. The index in this case might count some other information then entropy or might not be consistent. 2 Then, we study supersymmetric AdS 6 black hole solutions with other horizon geometries by considering D4-branes wrapped on Kähler four-cycles in Calabi-Yau fourfolds and on Cayley four-cycles in Spin (7) manifolds. We believe these are all possible four-cycles on which D4-branes can wrap. A product of two Riemann surfaces falls into a special case of Kähler four-cycles in Calabi-Yau fourfolds. We derive the supersymmetry equations, and obtain new supersymmetric AdS 2 solutions for each case. 3 We comment on the comparison with the recent field theory results. The topologically twisted index can be written as the contour integral of meromorphic differential form in variables parametrizing the Cartan subgroup and subalgebra of the gauge group, summed over the lattice of gauge magnetic fluxes, m, on the internal manifold [17,18]. Recently, topologically twisted index of 5d USp(2N ) gauge theory on Σ g 1 ×Σ g 2 ×S 1 was calculated at finite N by two independent groups, [19] and [20], and their calculations agree. When considering the large N limit, they both employed a conjecture to extremize the prepotential in order to get a saddle point distribution for dominant eigenvalue distribution. In [20], by considering the non-zero magnetic fluxes as a subleading contribution, the contribution to the twisted index from zero magnetic fluxes, m = 0, was evaluated. As we explain in detail below, it matches the gravitational entropy of the AdS 2 solution in [14] which is expected to be incorrect, and it counts the half of the full contribution to the twisted index. However, in [19], instead of setting the magnetic fluxes to zero, they extremized the twisted superpotential in order to get a saddle point distribution for the fluxes as well. In this paper, we will show that the full gravitational entropy of asymptotically AdS 6 black holes with AdS 2 ×Σ g 1 ×Σ g 2 horizon matches the topologically twisted index in the large N limit, only when the contributions from non-zero gauge theory magnetic fluxes are accounted as it was done in [19].
In section 2, we review F (4) gauged supergravity. In section 3, we study supersymmetric black holes with AdS 2 × Σ g 1 × Σ g 2 horizon by considering D4-branes wrapped on two 2 We would like to thank Alberto Zaffaroni for discussion on this point. 3 These cases were previously studied in [14] as D4-branes wrapped on Kähler four-cycles in Calabi-Yau threefolds and on co-associative four-cycles in G2 manifolds. However, as they have not turned on the two form gauge potential which is needed to have a consistent set of supersymmetry equations and to satisfy the equations of motion, we conclude that their equations and solutions are not correct.

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Riemann surfaces. We derive the supersymmetry equations, find a new AdS 2 solution, and calculate entropy of the black holes. We also present the full black hole solution numerically. In section 4, we consider more horizon geometries by studying D4-branes wrapped on Kähler four-cycles in Calabi-Yau fourfolds and on Cayley four-cycles in Spin(7) manifolds. In section 5, we conclude. The equations of motion of F (4) gauged supergravity are presented in appendix A.

F (4) gauged supergravity in six dimensions
We review SU(2)×U (1)-gauged N = 4 supergravity in six dimensions [2]. The bosonic field content consists of the metric, g µν , a real scalar, φ, an SU(2) gauge field, A I µ , I = 1, 2, 3, a U(1) gauge field, A µ , and a two-form gauge potential, B µν . The fermionic field content is gravitinos, ψ µi , and dilatinos, χ i , i = 1, 2. The field strengths are defined by The bosonic Lagrangian is given by where g is the SU(2) gauge coupling constant and m is the mass of the two-form gauge potential. The supersymmetry transformations of the fermionic fields are 3)

The supersymmetry equations
In this section, we obtain supersymmetric AdS 6 black holes with a horizon which is a product of two Riemann surfaces. We consider the metric, for the S 2 × S 2 background, and for the H 2 × H 2 background. The only non-vanishing component of the non-Abelian SU(2) gauge field, A I µ , I = 1, 2, 3, is given by for the S 2 × S 2 background, and for the H 2 × H 2 background, where the magnetic charges, a 1 and a 2 , are constant. In order to have equal signs for field strengths, we set opposite signs of the gauge fields for S 2 × S 2 and H 2 × H 2 backgrounds. We also have a non-trivial two-form gauge potential, B µν , and we will determine it later. We turn off the Abelian U(1) gauge field, A µ .

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The supersymmetry equations are obtained by setting the supersymmetry variations of the fermionic fields to zero. From the supersymmetry variations, we obtain where the hatted indices are the flat indices. The t-, θ 1 -, and θ 2 -components of the gravitino variations give (3.5), (3.6), (3.7), and the dilatino variation gives (3.8). The φ 1 -, φ 2components of the variations are identical to the θ 1 -, and θ 2 -components beside few more terms, We employ the projection conditions, where λ = ±1. Solutions with the projection conditions preserve 1/8 of the supersymmetries. By employing the projection conditions, we obtain the complete supersymmetry equations, (3.11)

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From (3.9) we also obtain the twist conditions on the magnetic charges, where k = +1 for the S 2 × S 2 background and k = −1 for the H 2 × H 2 background. 4 In the derivation of the supersymmetry equations, we determined the non-zero components of the two-form gauge potential, B µν . We determined the normalization by solving the equations of motion, The three-form field strength of the two-form gauge potential, G µνλ , vanishes identically. The supersymmetry equations satisfy the equations of motion. We present the equations of motion in appendix A. When we plug the twist conditions, (3.12), in the supersymmetry equations, we obtain where k = +1 for the S 2 × S 2 background and k = −1 for the H 2 × H 2 background. The supersymmetry equations in (3.14) are analogous to the equations for M5-branes wrapped on two Riemann surfaces in [21], and more recelty generalized in [22].

The AdS 2 solution and entropy of black holes
Now we will consider the N = 4 + theory, g > 0, m > 0. We find a new AdS 2 fixed point solution for the H 2 × H 2 background with k = −1, 5 When we consider the S 2 × S 2 background with k = +1, AdS 2 fixed point does not exist. 4 It is possible to have geometries like S 2 × H 2 for k1 = +1 and k2 = −1, or vice versa. One can easily generalize our supersymmetry equations and the twist conditions to that case. 5 The solution can also be presented as By employing the uplift formulae in [6], the AdS 2 solution can be uplifted to a solution of massive type IIA supergravity. We only present the uplift formulae for the metric, ds 2 10 = sin 1/12 ξX 1/8 ∆ 3/8 ds 2 6 + (3.17) and the dilaton field, Φ, where we define ∆ = X cos 2 ξ + 1 The solution in (3.16) describes the AdS 2 × H 2 × H 2 horizon of six-dimensional black holes. Moreover, when we consider the N = 4 + theory with g = 3m, there is a supersymmetric AdS 6 fixed point which is known to be dual of 5d USp(2N ) gauge theory in the large N limit. Recently, there has been development in calculating topologically twisted index of 5d USp(2N ) gauge theory on M 4 × S 1 by two independent groups, [19] and [20]. See the introduction for more details on their calculations. Analogous to the 3d gauge theory examples in [16][17][18], the entropy of the black holes could match the topologically twisted index of 5d USp(2N ) gauge theory on Σ g 1 × Σ g 2 × S 1 in the large N limit. Now we calculate entropy of asymptotically AdS 6 black holes with AdS 2 × H 2 × H 2 horizon. It can be easily generalized to AdS 2 × Σ g 1 × Σ g 2 horizon where g 1 > 1 and g 2 > 1.
Here Σ g is a Riemann surface of genus g with constant curvature. We would like to consider the AdS 6 fixed point in the N = 4 + theory by taking g = 3m. In order to have unit radius, L AdS 6 = 1, we set m = √ 2. 6 The Bekenstein-Hawking entropy of the black hole is given by 20) where L, vol, and G N are radius, volume, and the Newton's gravitational constant for the corresponding spaces, respectively. We used that the volume of Riemann surfaces with genus, g > 1, is 7 vol and, in the last equality, we used the value of the warp factor at our AdS 2 solution, e 4g = 2/3 3 . We can relate the gravitational entropy to the free energy of 5d SCFTs on S 5 by using the universal formula, 8

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and then entropy of the black hole is The free energy of 5d USp(2N ) gauge theory with N f flavors on S 5 in the large N limit is given by [25], Therefore, entropy of the black hole can be written by where g 1 > 1 and g 2 > 1. This nicely matches the topologically twisted index of 5d USp(2N ) gauge theory on Σ g 1 × Σ g 2 × S 1 in the large N limit calculated in [19]. As it was explained in the introduction, the contribution to the topologically twisted index with zero magnetic fluxes, m = 0, calculated in [20], counts only the half of the gravitational entropy.

Numerical black hole solutions
Now we present the full black hole solution numerically. The full black hole solution is an interpolating geometry between the asymptotically AdS 6 boundary and the AdS 2 × Σ g 1 × Σ g 2 horizon. We introduce a new radial coordinate, This kind of coordinate was introduced in [22]. Employing the supersymmetry equations, we obtain ∂ρ ∂r Then, the supersymmetry equations are In the r-coordinate, the UV or asymptotically AdS 6 boundary is at r = 0, and the IR or AdS 2 × Σ g 1 × Σ g 2 horizon is at r = ∞. In this ρ-coordinate, the UV is at ρ = +∞, and the IR is at ρ = −∞. We present the plot of the full black hole solution in figure 1. We have set m = √ 2 and g = 3m, and there is no free parameter left. Therefore, there is only one plot.

Black holes with other horizons
In this section, we obtain more black hole solutions with other horizon geometries by considering D4-branes wrapped on Kähler four-cycles in Calabi-Yau fourfolds and on Cayley four-cycles in Spin(7) manifolds. We believe these are all possible four-cycles on which D4-branes can wrap in F (4) gauged supergravity. D4-branes on two Riemann surfaces in the previous section fall into a special case of D4-branes on Kähler four-cycles in Calabi-Yau fourfolds. The analogous results of M5-branes wrapped on supersymmetric four-cycles were studied in [21,23].

Kähler four-cycles in Calabi-Yau fourfolds
We consider the metric, where M 4 is a Kähler four-cycle in Calabi-Yau fourfolds. The curved coordinates on the Kähler four-cycles will be denoted by {x 1 , x 2 , x 3 , x 4 }, and the hatted ones are the flat coordinates. For Kähler four-cycles in Calabi-Yau fourfolds, there are four directions transverse to D4-branes in the fourfolds. The normal bundle of the four-cycle has U(2) ⊂ SO(4) structure group. We identify U(1) part of the structure group with U(1) gauge field from the non-Abelian SU(2) gauge group, [23,26]. The only non-vanishing component of the non-Abelian SU(2) gauge field, A I µ , I = 1, 2, 3, is given by where the magnetic charges, a 1 and a 2 , are constant. The only non-vanishing component of the two-form gauge potential is

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We employ the projection conditions, where λ = ±1. Solutions with the projection conditions preserve 1/8 of the supersymmetries. By employing the projection conditions, we obtain the complete supersymmetry equations, with the twist conditions, where k determines the curvature of the Kähler four-cycles in Calabi-Yau fourfolds. A product of two Riemann surfaces considered in the previous section is a special case of Kähler four-cycles in Calabi-Yau fourfolds. When we identify g ≡ g 1 = g 2 in the supersymmetry equations for D4-branes wrapped on two Riemann surfaces, (3.14), we obtain the supersymmetry equations here, (4.5). By solving the supersymmetry equations, we find an AdS 2 fixed point solution which is identical to the one obtained in the previous section, (3.16).

Cayley four-cycles in Spin(7) manifolds
We consider the metric, where M 4 is a Cayley four-cycle in manifolds with Spin (7) holonomy. The curved coordinates on the Cayley four-cycles will be denoted by {x 1 , x 2 , x 3 , x 4 }, and the hatted ones are the flat coordinates. In order to preserve supersymmetry for D4-branes wrapped on Cayley four-cycles in Spin (7) manifolds, we identify self-dual SU(2) + subgroup of the SO(4) isometry of the four-cycle, with the non-Abelian SU(2) gauge group, [23,26]. The self-duality is defined by and we denoted the self-duality and anti-self-duality by + and −, respectively. For the self-dual part, components are identified by γx 1x2 = γx 3x4 , γx 1x3 = γx 4x2 , γx 1x4 = γx 2x3 . (4.10)

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The only non-vanishing components of the non-Abelian SU(2) gauge field, A I µ , I = 1, 2, 3, are given by where the magnetic charges, a 1 , a 2 and a 3 , are constant. The only non-vanishing component of the two-form gauge potential is We employ the projection conditions, where λ = ±1. Solutions with the projection conditions preserve 1/16 of the supersymmetries. By employing the projection conditions, we obtain the complete supersymmetry equations, with the twist conditions, where k determines the curvature of the Cayley four-cycles in Spin (7) manifolds. Now we will consider the N = 4 + theory, g > 0, m > 0. By solving the supersymmetry equations, we find a new AdS 2 fixed point solution for the negatively curved Cayley fourcycles with k = −1,  Now we present the full black hole solution numerically. The full black hole solution is an interpolating geometry between the asymptotically AdS 6 boundary and the AdS 2 × Cayley 4 horizon with negative curvature, k = −1. We introduce the radial coordinate, ρ, in (3.26), and solve the supersymmetry equations in ρ coordinate, as we did in section 3.3. We again set m = √ 2 and g = 3m. The full black hole solution is presented in figure 2.

Conclusions
In this paper, we studied supersymmetric AdS 6 black holes with various horizon geometries. We found asymptotically AdS 6 black holes with AdS 2 × Σ g 1 × Σ g 2 horizon with g 1 > 1 and g 2 > 1 and presented the full black hole solution numerically. We calculated the Bekenstein-Hawking entropy of the black holes, and found that it nicely matches the topologically twisted index of 5d USp(2N ) gauge theory on Σ g 1 × Σ g 2 × S 1 in the large N limit obtained in [19]. The contribution to the topologically twisted index with zero magnetic fluxes, m = 0, calulated in [20], counts only the half of the gravitational entropy. We also found black hole solutions by considering D4-branes wrapped on Kähler four-cycles in Calabi-Yau fourfolds and Cayley four-cycles in Spin (7) manifolds. For the near-horizon geometries we considered in this paper, we have shown that there should be non-zero two-form gauge potential, B µν , in order to have a consistent set of supersymmetry equations, and satisfy the equations of motion. For this reason, as explained in the introduction, we concluded that the equations and solutions for the corresponding cases in the previous study, [14], are not correct.
It would be interesting to study supersymmetric four-cycles in matter coupled F (4) gauged supergravity [27] along the line of [28], to obtain more examples of supersymmetric black holes in AdS 6 [29,30].

A The equations of motion
In this appendix, we present the equations of motion of F (4) gauged supergravity,