Supercharging superstrata

We construct a new class of smooth horizonless microstate geometries of the supersymmetric D1-D5-P black hole in type IIB supergravity. We first work in the AdS3 × S3 decoupling limit and use the fermionic symmetries of the theory to generate new momentum carrying perturbations in the bulk that have an explicit CFT dual description. We then use the supergravity equations to calculate the backreaction of these perturbations and find the full non-linear solutions both in the asymptotically AdS and asymptotically flat case. These new geometries have a simpler structure than the previously known superstrata solutions.


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1 Introduction and summary The thermodynamic entropy of certain extremal black holes was successfully explained by enumerating the microstates predicted by string theory [1][2][3]. In particular, the D1-D5-P black hole, which is a supersymmetric, 3-charge solution in type IIB string theory, has been an important arena for studying microscopic physics of black holes. This is partly because it allows a holographic description in terms of a two-dimensional CFT, called the D1-D5 CFT, which is under good theoretical control.
Although by now we understand the counting of black-hole microstates very well, their physical nature remains mysterious. The fuzzball conjecture [4][5][6][7] claims that blackhole microstates are made of stringy fuzz that is free of a horizon and singularities, and spreads over the size of the would-be horizon. The typical microstates of generic black holes such as the Schwarzschild black hole are expected to involve stringy modes and cannot be described within supergravity, the massless-mode truncation of the full string theory. However, constructing microstates in the full string theory is beyond the reach of our current technology and understanding.
The microstate geometry programme (see [8] and references therein) aims to construct as many black-hole microstates as possible within supergravity as smooth, horizonless geometries. The programme has been particularly successful for supersymmetric black holes, where a large number of microstate geometries have been explicitly constructed [9,10]. 1 It is still unclear how large a subset of all microstates is describable within supergravity but, even if not all microstates allow a supergravity description, explicit microstate geometries are important because they provide the only top-down, direct tool available for studying and understanding the microstate structure of black holes.
Superstrata [21][22][23][24][25] (see also [26]) represent the largest family of microstate geometries constructed thus far for the D1-D5-P black hole with known CFT duals and have various interesting features. The D1-D5-P black hole contains momentum (P) charge along an S 1 coordinatised by v, and superstrata contain v-dependent travelling waves corresponding to the P charge. As will be detailed below, superstrata are constructed based on a solutiongenerating technique whose holographic meaning is well-understood. Consequently, the CFT states dual to superstrata are explicitly known, which makes them an ideal setup for studying precision holography [27][28][29][30]. Superstrata also give interesting clues for the physical nature of typical microstates. Although the superstrata written down thus far are not typical microstates of the black-hole ensemble, they are expected to evolve into more JHEP03(2019)095 typical states when perturbed, and the endpoint of such a process is a subject of much physical interest [31][32][33][34][35][36][37].
In this paper, we present an explicit construction of an entirely new class of superstrata. They share the same features as the original superstrata [23][24][25], such as representing microstates of the D1-D5-P black hole and having dual CFT states. However, they are simpler than the original ones in that they involve a smaller number of non-trivial fields.
The original superstrata were constructed using the solution-generating technique as follows. First we take, as a seed, some 2-charge solution of linear supergravity around AdS 3 × S 3 , for which the dual CFT state |ψ is known. 2 Next, we act on it with the generators of the SU(1, 1|2) L × SU(1, 1|2) R (super)isometry group of AdS 3 × S 3 [11]. Specifically, we apply L −1 and J + 0 generators 3 of the bosonic subgroup SL(2, R) L × SU(2) L ⊂ SU(1, 1|2) L [23][24][25]. This process generates a new linear solution with non-vanishing third (P) charge. Acting on the seed m times with J + 0 and n times with L 1 generates the solution dual to the CFT state (J + 0 ) m (L −1 ) n |ψ . Finally, we use the structure of the BPS equations to complete the linear solution to a fully backreacted non-linear solution. In CFT, this final process corresponds to having the same excitation many times, namely, [(J + 0 ) m (L −1 ) n |ψ ] Nmn , with N mn ≫ 1. However, the supergroup SU(1, 1|2) L also includes fermionic generators G +A −1/2 , where A = 1, 2 is the index for an SU(2) B group related to the internal manifold. Therefore, alternatively, we can act with these fermionic generators on the seed (namely, "supercharge" it) to generate a completely new class of linear solutions. In order to get a bosonic solution, we need to act twice with fermionic generators. In addition to this, one can act on the newly obtained state with the bosonic symmetry generators to obtain a new state (J + 0 ) m (L −1 ) n G +1 −1/2 G +2 −1/2 |ψ . 4 The non-linear completion goes much the same way as before, and produces a new set of superstrata.
The supersymmetric solutions in supergravity are parametrised by a number of scalars and forms [23,[38][39][40]. In microstate geometries, these quantities get excited in non-trivial ways, representing the structure of the microstate. In the original superstrata, a scalar and a 2-form (which is related to the NS-NS B-field) get excited at linear order and, at quadratic order, more scalars and forms are turned on in a very specific way so that the combination that enters the metric is v-independent. This mechanism was crucial for the explicit construction of the geometry and was called "coiffuring" [41]. In contrast, in our new superstrata, at linear order, only the 2-form is excited and there is no scalar excited that must be cancelled by other scalars excited at higher order. Thus we will see that coiffuring is not necessary for the new superstrata and, consequently, they are simpler than the ones generated just by using bosonic symmetries. In hindsight, the existence of such a simple branch of superstrata could have been expected from the analysis of the excitation spectrum of linear supergravity around AdS 3 × S 3 [42][43][44][45]; see appendix C for details. However, we go beyond such linear analysis and construct fully non-linear solutions using the structure of the BPS equations.

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Due to their simplicity, studying the structure of the solution is easier for the new superstrata than for the original ones. For example, although the solution-generating technique can only produce asymptotically AdS 3 solutions, we can trivially extend the new superstrata to asymptotically flat solutions, as we do in section 6.3. In contrast, extending the original superstrata to asymptotically flat ones required a non-trivial step of solving differential equations [25]. Also, in the original superstrata, there was technical difficulty in constructing solutions that involves two modes with completely different quantum numbers (k 1 , m 1 , n 1 ), (k 2 , m 2 , n 2 ) [25]. The simple setup of the new superstrata may shed light on this technical point.
Investigating physical aspects of this new class of superstrata, such as the integrability of the geometry [35] and their precision holography [27][28][29][30] would be very interesting. As mentioned above, possible instabilities of microstate geometries have attracted much interest lately [31][32][33][34][35][36][37]. In particular, it has been argued [31] that supersymmetric microstate geometries are non-linearly unstable when a small amount of energy is added, leading to a formation of a near-extremal black hole. The metric of the original superstrata in the asymptotically-flat setting [25] has no isometry in the v direction, which violates one of the assumptions in the analysis of [31]. However, the asymptotically-flat version of the new single-mode superstrata (6.16) is v-independent metrically, and it would be interesting to examine their possible instability and its endpoint.
The structure of the current paper is as follows. In section 2 we give a brief description of the D1-D5 CFT, which is dual to the supergravity picture, and present the family of CFT states whose dual gravitational geometries we want to construct. In section 3 we then go to the supergravity side and introduce the setup of BPS equations governing the ansatz quantities that define the fields of our solutions. We then introduce the two-charge geometry which we will use as a seed in our solution-generating technique and present the superstrata that were previously constructed in [23,25]. In section 4 we construct the Killing spinors of empty global AdS 3 × S 3 × T 4 and use them to generate the fermionic variations of the supergravity fields, which are given in section 5. There we construct the new superstrata solutions to linear order in the perturbation parameter, corresponding to an infinitesimal deformation of AdS 3 × S 3 × T 4 . We then derive the fully backreacted, nonlinear solution in section 6, where we also discuss the asymptotically flat extension, calculate the conserved charges obtained from the geometry, and compare them to the conserved charges calculated on the CFT side. In section 7, we collect formulas for the new superstrata and, in addition, present two families of solutions for which all the excited scalars and forms can be written down in an explicit way. The reader who is interested in the explicit form of the superstrata geometry may find this section useful. Appendix A summarises our convention for type IIB supergravity, in particular, supersymmetry variations, spinors, and gamma matrices. In appendix B, we discuss some technical aspects of the supersymmetry variations that are not fully covered in the main text. In appendix C, we summarise the spectrum of linear supergravity around AdS 3 × S 3 worked out in [42]. This predicts the structure of excited fields in the new superstrata that we found in this paper, and further suggests other simple kinds of superstratum that would be interesting to investigate. In appendix D, we work out the map between the Killing spinors in the NS-NS coordinates presented in the main text and the ones in the RR coordinates.

JHEP03(2019)095 2 A CFT starter
According to the AdS/CFT duality, type IIB string theory on AdS 3 × S 3 × M (where M can be either T 4 or K3) is equivalent to a 2D SCFT with N = (4, 4) supersymmetry, called the D1-D5 CFT. 5 Besides Virasoro's symmetry, this SCFT has two sets of fermionic generators G αA ,Gα A and of bosonic currents J i ,Jī that together form a holomorphic and an anti-holomorphic copy of the small N = 4 superconformal algebra. The Greek indices α andα are in the fundamental representation of SU(2) L and SU(2) R respectively: this SU(2) L ×SU(2) R is the R-symmetry of the theory. The indices i andī are the triplet indices of SU(2) L and SU(2) R , respectively. The index A is in the fundamental representation of another SU(2) B , which acts as an outer automorphism on the superalgebra. Similar to N = 4 Super-Yang-Mills theory, this holographic SCFT also has a free locus in its moduli space where it can be described by a collection of free fields: 6 ∂X AȦ (r) , ψ αȦ (r) in the holomorphic and similarly∂X AȦ (r) ,ψαȦ (r) in the anti-holomorphic sector, where r = 1, . . . , N , so the total central charge is c = 6N . Notice that the new type of indicesȦ, appearing on the free fields, belongs to a SU(2) C that is not part of the symmetry group of the theory. Since the bosonic fields are in the (2, 2) representation of SU(2) C ×SU(2) B , one can think of this group as acting on the tangent space of the target space M of one boson. The free locus is described by N copies of the elementary fields which need to be treated as identical, so the full target space is the orbifold M N /S N , where S N is the symmetric group acting on the index (r) labelling the copies.
In the following we will use the anomaly-free part of the small N = 4 superconformal algebra in the NS-NS sector, with n, m = −1, 0, 1 and s, r = ± 1 2 , while (σ j ) α β are the Pauli matrices and all SU(2) indices are lowered/raised with the ǫ satisfying 7 ǫ 12 = ǫ +− = ǫ 21 = ǫ −+ = 1. When M is T 4 , there are additional U(1) currents that in the free theory description are simply N r=1 ∂X AȦ (r) and N r=1∂ X AȦ (r) . They will play no role in our discussion which is valid for both the T 4 and K3 cases.
In the NS-NS sector, SL(2, C)-invariant vacuum |0 satisfies L n |0 =L n |0 = 0 for any n ≥ −1 and G αA r |0 =Gα A r |0 = 0 for r ≥ −1/2 which implies J i n |0 =Jī n |0 = 0 for n ≥ −1. In what follows a particular kind of state, called an anti-chiral primary state, will play the central role in the construction of new superstrata solutions. An anti-chiral state 5 See e.g. [46,47] for reviews of the D1-D5 CFT. 6 In order to have a free theory description of the K3 case one can as usual consider the orbifold limit K3 = T 4 /Z2, where the fields with an odd number ofȦ indices are odd under Z2. See e.g. [25] for a discussion on the moduli space and the position of the free orbifold point in it. 7 We will use α = +, − and A = 1, 2 to highlight the difference between the R-symmetry and the outer automorphism indices.

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|s satisfies L n |s = 0 , n ≥ 1 ; G αA r |s = 0 , r ≥ 1 2 ; J − n |s = 0 , n ≥ 0 ; J + n |s = J 3 n |s = 0 , n ≥ 1 ; L 0 |s = −J 3 0 |s = h|s , where, as usual, J ± = J 1 ± iJ 2 . A simple example of such a state in the free theory is which has h =h = 1/2. There is a family of anti-chiral primary operators 9 Σ −− [k] with h =h = k−1 2 that, at the free locus, live in the twisted sectors of the orbifold S N mentioned above. These operators change the boundary conditions of the elementary fields. For instance when acting on the vacuum they link together k copies of the elementary fields into a single object that we call a "strand". In the following, we will use the anti-chiral where a strand of length k is further excited by a holomorphic and an anti-holomorphic elementary fermionic field and, for the corresponding states, we introduce the notation Acting with J + 0 , L −1 and G +A where m ≤ k − 2q, q = 0, 1, otherwise the state is trivially zero, while n = 0, 1, 2 . . . can be any non-negative integer. The eigenvalues (h, j) of L 0 and J 3 0 are h = k 2 + n + q and j = − k 2 + m + q, while (h,j) are unchanged. Notice that, due to the commutation relations (2.1), the order of the operators in (2.6) is immaterial. The combination in the parenthesis (weighted by q) is chosen so as to make the states |k, m + 1, n + 1, 0 NS and |k, m, n, 1 NS orthogonal, which means that, under the AdS/CFT dictionary, they will correspond to two independent supergravity perturbations. It is straightforward to check this by using the commutation relations (2.1). It is easier to start with the n = 0 case: 8 In our conventions the OPEs between the elementary fields are and G αA = N r=1 ψ αȦ (r) ∂X AḂ (r) . Similar relations hold for the anti-holomorphic sector. 9 The subscript [k] in the square parenthesis refers to the order of the twisted sector where the operator under discussion lives.

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This shows that L 1 |k, m, n, q NS ∼ |k, m, n − 1, q NS , so we can recursively prove the orthogonality of |k, m + 1, n + 1, 0 NS and |k, m, n, 1 NS for general n. Finally notice that the state |1, 0, 0, 1 NS is trivial 10 since it has zero norm and so all the states |1, 0, n, 1 NS are zero since they are constructed from |1, 0, 0, 1 NS by dressing it with powers of L −1 .
The final CFT ingredient we need is the possibility of realising the superalgebra in equivalent ways by taking the spectral flow of the generators (here we follow the conventions of [48]) and similarly for the anti-holomorphic sector. When the spectral flow parameter ν takes half-integer values, the theory is in the RR sector, and in particular, for ν =ν = −1/2, an anti-chiral primary state flows to RR ground state with h R = c/24 and j R = −h NS + c/12 (since j NS = −h NS for anti-chiral primary states). Thus, after this spectral flow, the states in (2.6) become excited RR states that we denote as where we used c = 6N and used that the NS-NS vacuum state |0 NS goes into the RR ground state |++ .
In this work we focus on protected RR states that are dual to smooth supergravity solutions. A nice class of such states is obtained by starting from a NS-NS multi-particle state which is the product of N b copies of (2.6) and then by performing the spectral flow to the RR sector mentioned above. In this paper we consider states involving just one type of excitation, dual to a single-mode superstrata solution, which in the RR sector then take the following form: (2.10) To be precise, the CFT states of this type are written as a coherent sum of terms involving a different number elementary excitations (2.6), but in the large N limit the sum is sharply peaked [49] and (2.10) represents the dominant term in the sum. For a discussion of this point in the context of three-charge states, see [25] and reference therein. Here it is sufficient to say that the coherent sum with a peak at (2.10) is defined in terms of two continuous parameters a 2 and b 2 , related to N a and N b respectively which determine also the dual gravity solution. Such a coherent sum of CFT states will have charges equal to the those of the dominant term (2.10). These charges are given by the eigenvalues of the operators L 0 ,L 0 , J 3 0 andJ 3 0 which are equal to respectively, and, as we will see in section 6.4 these results will match precisely the momentum and the angular momenta of the dual supergravity solution.

JHEP03(2019)095 3 Supergravity setup
Our final goal is to find the supergravity solutions dual to the CFT states (2.6) and (2.10).
As an illustration in this section we focus on the q = 0 case, i.e., we review the original superstrata [23][24][25], which only involve bosonic generators. In later sections we will generalise this approach to the q = 1 case, the new superstrata, which involve fermionic generators.

The BPS ansatz
We work in Type IIB string theory on R 1,4 × S 1 × M, where the internal space M is either K3 or T 4 . The D1-D5-P black hole is 1/8-BPS, which means that it preserves 1/8 of the total 32 supercharges. All of its microstates must also preserve the same amount of supercharges, meaning that all of them are 1/8 BPS. Such solutions of type IIB supergravity that are in addition independent of M are described by the following ansatz [40,48] We have defined new asymptotically null coordinates u and v as where t is the time coordinate and y parametrises the S 1 , which has total length 2πR y . These new coordinates can be thought of as world-volume coordinates of the dual CFT. In the above ansatz, ds 2 10 denotes the string-frame metric of the ten-dimensional spacetime, and ds 2 6 denotes the Einstein-frame metric of the six-dimensional spacetime, which is a fibration over a 4-dimensional base B with metric ds 2 4 which may depend on v. The ansatz includes scalars Z 1 , Z 2 , Z 4 , F; one-forms β, ω, a 1 , a 2 , a 4 ; two-forms γ 1 , γ 2 , δ 2 ; and a threeform x 3 , all on B. These quantities can depend on the coordinates of B and on v, but JHEP03(2019)095 supersymmetry requires them to be independent of u. The RR potentials C p can have an extra term proportional to a four-form C on B, but it has been set to zero by using the gauge symmetries discussed in [23].
The advantage of the above ansatz is that the functions and forms used to express the field content of the theory obey BPS differential equations which one can organise into layers and solve in successive steps, using the solutions to the previous layer as sources in the next one. The equations have three layers, which we call the zeroth, first, and second. The zeroth level gives the equations for the base space metric ds 2 4 and one-form β. This system of equations is non-linear and hard to solve. Hence we make an assumption that the base space B is R 4 equipped with a flat metric ds 2 4 and that the one-form β is v-independent. With these two assumptions, the zeroth-layer equations reduce only to the self-duality condition of β on the base space, dβ = * 4 dβ, (3.4) where * 4 denotes the Hodge dual operator on B = R 4 . The assumption of the simple base provides us with a tractable class of solutions that can be explicitly written down, although we must keep in mind that it limits how generic our solutions are. The first-layer equations are a set of linear equations where we have introduced gauge invariant 11 two-forms and defined a gauge covariant differential operator where d 4 denotes the exterior derivative on the base space. The above equations describe three systems of equations for (Z 1 , Θ 2 ), (Z 2 , Θ 1 ), and (Z 4 , Θ 4 ), which have the same structure. Thus if, for example, we find a solution for the pair (Z 4 , Θ 4 ) then we have also found a solution for the other two pairs. It is important to note that once we have solutions to the zeroth-layer equations, the first-layer equations can be fully solved at least in principle. The second layer of equations is a set of linear differential equations that determine F and ω. These are of special interest as their long distance behaviour allows us to read off the momentum and angular momentum charges of the geometry. The two equations are (3.8b) 11 Invariant with respect to the gauge transformations given in (2.14) of [23].

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The solutions to the first-layer equations serve as sources on the right-hand side of the differential equations. It is also important that these sources appear quadratically in the right-hand side of second-layer equations. Hence any first-order perturbation in the firstlayer quantities becomes a second-order perturbation in the second layer. This fact is useful in the solution-generating technique that is used to build new solutions.

Seed solution
The construction of three-charge black holes via the superstratum technology begins with a two-charge seed solution. All two-charge solutions are known [28,[50][51][52], and can be obtained by a systematic procedure using an auxiliary curve in R 8 , which determines the values of the ansatz quantities of (3.1). For a short overview of the construction of twocharge solutions and especially the one used in the subsequent sections, see, for instance, appendix A of [23]. The seed solution used for the construction of superstrata solutions is given as a perturbed round supertube solution [28]. We start off by parameterising the base space R 4 with a new set of coordinates related to the Cartesian ones by where θ ∈ [0, π 2 ] and φ, ψ ∈ [0, 2π). The ansatz quantities in these coordinates are given by 12 ds 2 4 = (r 2 + a 2 cos 2 θ) dr 2 r 2 + a 2 + dθ 2 + (r 2 + a 2 ) sin 2 θ dφ 2 + r 2 cos 2 θ dψ 2 , (3.10a) where we have introduced Σ ≡ r 2 + a 2 cos 2 θ , and the parameter k is a positive integer. We take the parameter b to be small and only keep O(b) terms. Hence we can think of the solution (3.10) as a combination of the background supertube (b = 0) [53][54][55], with an added perturbation (b = 0), which turns on JHEP03(2019)095 form fields B 2 , C 0 , and C 4 . Because Z 4 appears only quadratically in the 10-dimensional metric (3.1a), the perturbation does not change the metric at linear order in b. In the same approximation the parameter a is related to the D-brane charges Q 1 and Q 5 via It is not difficult to check that the above ansatz satisfies the BPS equations (3.5) and (3.8) to linear order. One could consider the finite b version of the above seed solution [23], but that is not necessary for our purposes. Performing a coordinate transformation 12) one finds that the six-dimensional metric becomes (3.13) which is that of global AdS 3 × S 3 with radius R 2 AdS = √ Q 1 Q 5 . Therefore, our seed solution represents AdS 3 × S 3 × T 4 with a linear perturbation on top of it. On the CFT side, this corresponds to the NS-NS vacuum with a small excitation on top. 13 Since the NS-NS vacuum is invariant under the action of SL(2, C) ∼ = SL(2, R) L × SL(2, R) R and SU(2) L × SU(2) R transformations, acting on the excited state with the generators of these symmetries generates a new state, which is again the NS-NS vacuum with a different small excitation added to it. Performing the corresponding transformations on the seed solution on the gravity side similarly generates pure AdS 3 × S 3 × T 4 with a different linear perturbation on top of it. This new solution will again satisfy the BPS equations and, in addition to it, we will precisely know the CFT state dual to the new geometry.
It is important to note that the transformation (3.12) involves a change of the coordinates t and y, which parametrise the boundary region of AdS 3 . This means that this transformation also affects the dual CFT theory. In fact this transformation is dual to the spectral flow transformation that changes the RR sector into the NS-NS sector on the CFT side (2.8). For that reason we will refer to the coordinates (r, t, y, θ, φ, ψ) as the RR coordinates and (r, t, y, θ, φ, ψ) as the NS-NS coordinates.
At this point we make the first identification between the supergravity solution and a dual CFT state. Using the standard AdS/CFT dictionary the seed (3.10) expressed in the RR coordinates is dual to a RR ground state. After performing the spectral flow transformation (3.12) to the NS-NS coordinates, the geometry is dual to an anti-chiral primary with the conformal dimensions h = h = k 2 and j = j = − k 2 . We thus identify the supertube ansatz expressed in the NS-NS coordinates is dual to the state (2.5). As usual, the gravity and the free CFT descriptions are valid in different points of the moduli space, so the dictionary mentioned above is meaningful when applied to protected quantities such as the 3-point correlators [56].

Original superstrata
This work follows up on the work of [23,25,48], where new superstrata solutions were obtained by acting on the seed solution (3.10) with the gravity realisations of the bosonic symmetry generators J + 0 and L −1 , thus finding the geometries dual to the CFT states (2.6) with q = 0. Below we will review the construction of this class of superstrata.
As mentioned above, the background is invariant under the action of SL(2, R) L × SL(2, R) R and SU(2) L × SU(2) R , while on the other hand the perturbation is not. Acting on the perturbed geometry with these generators will give us a new perturbed geometry. Focusing on the left sector of the theory and the corresponding symmetry groups SL(2, R) L × SU(2) L , one can show that the generators of these symmetries can be explicitly realised in the in the NS-NS coordinates as [25,43] 14) which can be shown to satisfy the algebra (2.1).
Acting on the seed solution (3.10) with (3.15) m times and with (3.14) n times leaves all ansatz quantities unchanged at linear order. 14 in b 4 ∼ b except for the function Z 4 and the two-form Θ 4 , which are now given by where we have introduced the notation

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and we have expanded ϑ k,m,n on a basis of self-dual two-forms Ω (i) (i = 1, 2, 3) on R 4 , given by: One of the important aspects of these solutions is that they now depend on the variable v, unlike the seed solution (3.10).
The above solution-generating technique allows us to generate a family of solutions, parametrised by the quantum numbers (k, m, n). Although the above solutions (3.16) only involve one mode at a time, using the linearity of the first-layer BPS equations, we can write down the general solution given by an arbitrary superposition of modes with different quantum numbers. This superposition will not only solve the first-layer BPS equations for the Z 4 and Θ 4 , but also for the other two pairs (Z 1 , Θ 2 ) and (Z 2 , Θ 1 ), because the structure of their equations is identical. Hence the general class of solutions with q = 0 for the firstlayer equations are given by (3.20) where Z 1 and Z 2 also include the zero modes, which appear in the seed solution. In these superpositions the coefficients b k,m,n I are still taken to be infinitesimal. In this case they generate second-order source terms on the right-hand side of the second-layer BPS equations, which govern the change of F and ω. Thus to linear order in the perturbation parameter, these two ansatz quantities remain the same. This infinitesimal solution corresponds to an infinitesimal deformation of the empty global AdS 3 × S 3 × T 4 spacetime.
However, we can again use the linearity of the first-layer BPS equation to make all the coefficients b k,m,n I finite, and the solution (3.20) will still remain a solution to the first-layer equations. With the coefficients being finite, we have non-vanishing source terms on the right-hand side of the second-layer BPS equations. Solving these represents a challenge. In [25], a general solution to the second-layer equations for single-mode superstrata was found. These solutions correspond to configurations with a single non-trivial coefficients b k,m,n 4 in (3.20). The lesson from the non-linear solution-generating technique employed in [40,48] is that the descendant states have b k,m,n 2 = 0 for all values of k, m, n and this is also the case for the single-mode superstrata, where one can consistently set b 2 = 0 [25]. Furthermore, b 1 was determined by "coiffuring", which in the single-mode case requires that the v-dependent source terms on the right-hand side of second-layer equations vanish. In the case of b 2 = 0, this corresponds to setting b 1 = b 2 4 , thus having the solutions to the JHEP03(2019)095 first layer given by By using these terms in the source terms of the second-layer equations, one finds that the second-layer quantities are given by where we further decompose One can show that the solutions for the second-layer equations are given by where the function F 2k,2m,2n is defined in (6.7), and the functions ν orig k,m,n are given by differential equations [25, (4.13)], and can be solved for each case individually. We have put the superscript "orig" to distinguish these original superstrata solutions from the new superstrata we are presenting below. The solutions obtained this way are asymptotically AdS 3 × S 3 × T 4 . To obtain asymptotically flat solutions, one needs to add "1" to the warp factors Z 1 and Z 2 . This alters the right-hand side of second-layer equations and induces new v-dependent terms into F and ω [25]. As it will turn out that our new superstrata do not generate these additional v-dependent terms in the case of asymptotically flat case, the asymptotically flat extension of the new solutions will be simpler than those of the original superstrata.

Killing spinors of the AdS 3 × S 3 background
In the previous section, we reviewed the construction of the original superstrata, which are dual to the states (2.6) with q = 0 and are generated by the supergravity realisation (3.14) and (3.15) of the bosonic generators J + 0 and L −1 . We now proceed to the construction of new superstrata, which have q = 1 and involve fermionic generators G +A . In supergravity, these fermionic generators correspond to the Killing spinors of the AdS 3 × S 3 × T 4 background. To begin with, in this section, we work out the explicit form of these Killing spinors, and give a precise map between their components and the fermionic generators G αA ± 1 2 in the CFT.

Supersymmetry variations
The supersymmetry variations for the dilatino λ and the gravitini fields ψ M in type IIB supergravity are given by 15 see (A.5) and (A.6) for our conventions on the form fields. In type IIB supergravity, each fermionic field appears in two copies, which we combine into a doublet ǫ ≡ (ǫ 1 , ǫ 2 ). The Pauli matrices σ i in the variations above act on the doublet indices, which will be made explicit in the following calculations when relevant. The variations (4.1) hold in a generic coordinate system in Type IIB supergravity. In our previous discussion, we have introduced two parametrisations of the unperturbed background: the NS-NS and the RR coordinates.
In what follows we will focus on the NS-NS description and derive an explicit expression for the Killing spinors (4.11), while in appendix D we derive the Killing spinors (D.7) in the RR coordinates and present the map between the two sets of solutions.
As mentioned before, in the seed (3.10), the metric, the dilaton, and In the NS-NS coordinates, the O(b 0 ) fields are the metric and On the other hand, the field strengths are . Therefore, the supersymmetry variations (4.1) for the seed solution (3.10) split into the JHEP03(2019)095 In this section, we are interested in the Killing spinors in the unperturbed (b = 0) background, which is nothing but AdS 3 ×S 3 ×T 4 . In the NS-NS coordinates its metric takes the form (3.13). We will work in the u, v coordinates (3.3), in which the metric becomes (4.5) which suggests the following choice of 10-dimensional vielbeine where x k , k = 6, 7, 8, 9 are the coordinates of the internal T 4 . With this choice the metric can be written as JHEP03 (2019)095 with a = r, θ, φ, ψ, 6, 7, 8, 9. The variations (4.4a) and (4.4b) can be written out explicitly as In these equations we have made the doublet index of the fermionic fields explicit. We have only given the variations for δλ 1 0 and δψ 1 M,0 , as the variations for δλ 2 0 and δψ 2 M,0 can be obtained simply by interchanging the doublet indices 1 ↔ 2 on all fermions in the above variations.

The Killing spinors
Killing spinors of the AdS 3 × S 3 × T 4 background are non-trivial spinors that satisfy the equations We find that the spinors that solve the equations (4.9) are given by where in the above spinors, the following definitions are used 16 and we have defined The spinors ζ ± , ζ ± are constant spinors that do not depend on any coordinates. As standard in type IIB supergravity, the ǫ 1,2 in (4.10) are Majorana-Weyl spinors. The Weyl condition is with Γ (10) ≡ Γ uvrθ φ ψ6789 . In our convention in which the charge conjugation matrix is C = Γ t , the Majorana condition reads We can now spell out the constraints following from (4.14) on the spinors in (4.10) and (4.11). The factors Y ± (θ, φ, ψ) and R ± (r) are real functions containing the explicit dependence of the spinors on the angular and radial parts respectively. Then in order for ǫ 1,2 to be real, spinors ζ ± , ζ ± must satisfy This means that ζ ± and ζ ± are complex. On the other hand, ξ(v), η(v), ξ(u) and η(u) are real spinors. Therefore, ξ(0), η(0), ξ(0) and η(0) are constant, real spinors, each containing 4 independent real degrees of freedom and can be used to parametrise the variations. Furthermore the dilatino variation and the variation in the T 4 subspace impose All spinors in (4.10) and (4.11), ξ, ξ, η, η, ζ ± , ζ ± , must satisfy the conditions (4.13) and (4.16). In addition, they have the following chirality for the matrix Γ uv :

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As mentioned above each one of η, η, ξ, ξ contains 4 real degrees of freedom. On the other hand, each one of ζ ± , ζ ± contains 4 complex degrees of freedom, but only half of them are independent. Therefore, either way, each spinor ǫ 1,2 contains 8 real degrees of freedom, combining to 16 in total. This is what we expected, as global AdS 3 × S 3 should preserve half of the total 32 supercharges.
In order to generate new solutions, we need to identify the spinor components that correspond to different modes of the fermionic generators G αA . We will only be interested in generating left-moving excitations, which are generated by G and not G, hence we will limit ourselves only to the discussion around the left-moving sector. However, the discussion on the right-moving sector is completely analogous. The relation between the supergravity Killing spinors ζ αA ± and the CFT supercurrent G αA can be encoded in terms of the projectors where J ψ is defined in (A.18a). We leave the discussion of this point to appendix A.3 and here quote just the final result With this identification we can proceed to generate the supergravity solution corresponding to the state (2.6) in CFT.

Fermionically generated superstrata: linear analysis
In this section we derive a linearised classical solution to the supergravity equations using the Killing spinors for AdS 3 × S 3 × T 4 obtained in the previous section. We do so by performing two supersymmetry variations, generated by the spinors corresponding to G αA , on the b = 0 seed solution (3.10). Single variations of bosonic fields vanish, as these are proportional to the fermionic fields, which are set to zero for classical supergravity solutions. Double variations of the bosonic fields, however, are non-vanishing, as these include terms which are proportional to the variations of the fermionic fields. Note that, by definition, Killing spinors are non-trivial spinors for which the variations of fermionic fields vanish. However, here we will use the Killing spinors for the unperturbed case (b = 0) on the perturbed background (b = 0), which will generate fermionic variations that are non-vanishing. We will limit ourselves to terms at linear order in parameter b. Using these non-vanishing fermionic variations we can generate new solutions at linear order in the parameter b. This section will give a step-by-step procedure of how to obtain the new solutions. We begin by presenting the variations of the fermionic fields of the seed solution, generated by the Killing spinors (4.10). We then present the double variations of the bosonic fields generated, thus obtaining the solution dual to the state G +1 In this derivation we treat the complex spinors ζ αA + and ζ αA − as independent, although they really are not, due to the relation (4.15). Because of this, the spinors ǫ 1,2 become complex and we will obtain JHEP03(2019)095 a complex-valued perturbation: as usual, at the linear level, we can derive a standard supergravity solution by taking the real part of the final result. While this is indeed a new solution to the first-layer BPS equation it is not linearly independent from the ones already known, as discussed in section 2. We therefore present the new, linearly independent solution, dual to the state G +1 and further give the solution dual to the state (2.6) with q = 1.

Variations of fermionic fields
As a preliminary step, we use the Killing spinors found in the previous section to calculate the supersymmetry variations of the fermionic fields. The result can be used later when we consider double variations of bosonic fields. Furthermore, it also serves as a consistency check of the identification (4.19) between the fermionic generators in supergravity and CFT.
As discussed in previous sections, the seed solution (3.10) expressed in the NS-NS coordinates is dual to an anti-chiral primary state, which should be annihilated by . According to the identification (4.19), this implies that the supersymmetry variation of the seed by ζ −A − will vanish while the supersymmetry variation by ζ +A − will not. In performing this check, we set ζ αA + = 0 and look at the variations of the fermionic fields generated by the components in the spinor ζ αA − . With this choice, the Killing spinor (4.10) simplifies to The dilatino variation generated by this spinor is given by This expression is correct for a generic component ζ αA − . However, as discussed above, this variation should distinguish between the ζ +A − and the ζ −A − components of the spinor. Indeed, this is the case here, as one can see from the factors that contain the gamma matrices with components along S 3 . Using the definition of Y + in (4.11) one can show that because, when we commute the factor in the brackets through Y + , we generate a projector P + S , which projects out the ζ −A − component. Therefore, as expected, the supersymmetry variation of the seed by ζ −A − vanishes, while the supersymmetry variation by ζ +A − does not. The variations of the gravitino components ψ M are calculated in the same manner and discussed in appendix B.

Solution-generating technique
The first step to finding the geometry dual to the state (2.6) with q = 1 is to find the geometry dual to G +1 fields. These variations generically have two kinds of terms: either they are proportional to fermionic fields or the variation of fermionic fields. In a classical solution, fermionic fields vanish and hence we are left only with the second type of terms. Using the variations summarised in appendix A, we get that, for example, the variation of the axion field C 0 is given by where δ denotes the variation generated by spinors ǫ 1,2 and δ ′ denotes the variation with different spinors ǫ ′1,2 . In our case the constant components of these spinors will be ζ +1 − for the variation δ and ζ ′+2 − for the variation δ ′ . Following the procedure of [23,25] we are interested in calculating the infinitesimal deformation from the seed solution in the ansatz function Z 4 and the two-form Θ 4 . The physical fields in which these two quantities are appearing are the axion C 0 and the NS-NS gauge B-field, so we are interested in their variations. Since these two calculations are analogous, we will only present the detailed calculation for the axion field, while the results of the B-field can be found in appendix B.
As mentioned at the beginning of this section, because we treat complex spinors ζ αA + and ζ αA − as independent, the spinor ǫ becomes complex. This is justified with the understanding that we will take the real part in the final result. In the intermediate calculations, although ǫ 1,2 are really complex, we still treat them as real spinors. In writing down (5.4), we used the relation (A.11), which is valid only for real (Majorana) spinors, in order to rewriteǭ appearing in the formula (A.1d) in terms of ǫ T . Another way to justify this manipulation is that, because the first variation parameter ǫ and the second one ǫ ′ are on an equal footing, it is not possible for ǫ to enter in the variation δ ′ δC 0 being complex conjugated and ǫ ′ without being complex conjugated. They must both enter without being complex conjugated, as in (5.4).
The variations we consider are generated by the Killing spinors (5.1). As mentioned above, the first variation is generated by the component ζ +1 − and the second by ζ ′+2 − . In this case, as we have seen in (5.1), we have ǫ 1 = −ǫ 2 . Furthermore, the variations are such that δλ 0 = 0 and δλ 1 b = δλ 2 b . With these, the axion variation (5.4) simplifies to We insert the spinor (5.1) and the variation (5.2) (since we use only ζ +A − we use the projection (5.3) in the variation) into this expression to obtain In the second equality we have used the properties of the Clifford algebra and the R ± functions together with the fact that Γ uv ζ αA − = −ζ αA − and hence Γ u ζ αA Furthermore, one uses the fact that (Γ rθ ) 2 = −1 to expand Γ rθ e −θΓ rθ = cos θ Γ rθ + sin θ.
Finally noting that due to the projector property (P + S ) T = P − S , we have (ζ +1 − ) T ζ ′+2 − = 0, which leaves us with the result (5.6). The calculation for the B-field follows along the same lines; see (B.7) for the final result.
After the inverse spectral flow coordinate transformation (the inverse transformation of (3.12)), one finds that the double variation leaves all ansatz quantities unchanged at linear order in b, except for Z 4 and Θ 4 , which are now given by 17 where we have again expanded Θ 4 in the self-dual basis (3.19). As in mentioned above, in the final result, we selected the real part of the perturbation. We also normalised the spinors as follows: aR y , which is natural since in our conventions, spinors have a mass dimension of −1/2 and so a spinor bilinear should have mass dimension −1 or should have units of length. One can check explicitly that the result (5.8a) satisfies the first-layer BPS equations (3.5).
To get a feeling for this solution we can compare it with the old superstrata solution (3.16), for (k, m, n) = (k, 1, 1), which is obtained by using the bosonic symmetry generators (3.15) and (3.14) only. The solutions are similar and this may not be unexpected, as they both introduce the same amount of momentum and angular momentum into the geometry. We notice that the form of the function Z 4 is the same, while Θ 4 slightly differs in the relative factors multiplying the basis elements Ω (i) .
As shown on the CFT side, the state G +1 The proper combination which contains the information about the new, linearly independent CFT state is given by the combination In order to write the supergravity solution dual to (5.9), let us briefly discuss the relation between the parameter b 4 in (3.16) and the original parameter b appearing in the seed solution. By keeping track of the overall normalisation when acting with bosonic generators (3.15) and (3.14), we have b 4 = (−1) n k (k+(n−1))! (k−m)! b. Because for m = n = 1 this gives b 4 = −k 2 b, one finds that the solution dual to the state (5.9) is given by the following new 17 The superscript f is to denote that these solutions are obtained by acting with fermionic generators only and hence the state that this solution is dual to is G +1

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linear perturbation The new solution has a vanishing Z 4 function, which means that both the axion field C 0 and also the component B uv of the B-field are vanishing. However, because Θ 4 is non-vanishing, the components of B µν with one leg in AdS 3 and one in S 3 are non-vanishing, which agrees with the spectrum calculated by [42]. For a brief summary of their results and the connection to the present work, see appendix C. One can show that Z 4 and Θ 4 given in (5.10) satisfy the first-layer of BPS equations (3.5). The solution is dual to the CFT state with quantum numbers (k, m, n, q) = (k, 0, 0, 1). Notice that for k = 1 both the above supergravity perturbation and the corresponding CFT state are trivial, which provides a further check on the identification proposed. We can generalise this approach and use the geometry (5.10) as a new seed solution and act on it with the bosonic symmetry generators (3.14) and (3.15) to obtain the geometry dual to the state (k, m, n, q = 1). One finds that the geometry dual to the state (2.6) with q = 1 is again unchanged at linear order from the original seed solution (3.10) in all the ansatz quantities except for 18 with ϑ k,m,n = ∆ k,1+m,1+n Σ r sin θ Ω (1) sinv k,1+m,1+n + Ω (2) + Ω (3) cosv k,1+m,1+n . (5.12) Again it is not difficult to show explicitly that these satisfy the first-layer BPS equations. Also in this more general case Z 4 remains trivial and the structure of Θ 4 is the same as in (5.10), apart from a change in the argumentv k,1+m,1+n of the trigonometric functions and in the quantum numbers in the ∆ k,1+m,1+n function.

Non-linear completion
In the previous sections we generated new solutions to the BPS equations at linear order in the perturbation parameter b. Since the first-layer BPS equations are linear, any linear combination of solutions (3.16) and (5.11), with an allowed combination of the quantum numbers (k, m, n), is also a solution of these equations. This general bulk configuration correspond to a CFT state containing various excitations (2.6) with different values of (k, m, n, q). Up to this point we have taken the coefficients b k,m,n I and b k,m,n I to be infinitesimally small, making any solution only an infinitesimal deformation of the empty AdS 3 × S 3 × T 4 space. In principle we could promote all these coefficients to be finite, 19 18 We reabsorb all overall normalisations in the parameter b k,m,n 4 . 19 See [25] for discussion on the technical difficulty in superposing modes with completely general (k1, m1, n1) and (k2, m2, n2).

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which corresponds, on the CFT side, to taking many copies of the same excitation. With the parameters b k,m,n I being finite, the scalars Z I and the two-forms Θ I become sources on the right-hand sides of the second-layer equations. Thus, once we have a finite solution to the first-layer equations, we can determine the deformation of F and ω from their seed values by solving the second-layer equations.
Here we will not tackle this general problem and will focus on a single-mode superstratum, i.e., we make a single, arbitrary mode coefficient to be finite and the solve the second-layer equations with the corresponding source terms. We find that a special feature of this new class of non-linear solutions is that their extension to asymptotically flat solutions is trivial. We close this section by calculating the conserved charges of the newly obtained solutions and comparing them to the CFT states (2.6) to find perfect agreement between the two results.

Solving the second-layer equations
The second-layer equations (3.8) are in general coupled second-order partial differential equations for the components of the anti-self-dual one-form ω and the scalar F. These quantities encode the information about the conserved charges of the geometry, i.e., the momentum charge Q p and the angular momenta J and J. As mentioned above, our goal here is to calculate the backreaction on ω and F that the new finite deformations cause on the geometry. We will limit ourselves to the case of single-mode superstrata involving the new q = 1 excitations, meaning that our initial ansatz for the finite first-layer solution is , which, in turn, is related to number of excitations (2.6) in the corresponding CFT state. We further simplify our ansatz by recalling that the bosonic descendants of an anti-chiral primary state have a trivial Θ 1 [48]. The same feature is shared by the bosonic superstrata obtained by using the excitations (2.6) with q = 0 [25]. We assume that a similar property holds also for q = 1 excitations and set to zero the coefficients b k,m,n 2 . Furthermore, in all previous work [23,25,60], the coefficients b k,m,n 1 were tuned in such a way that the singularity-causing vdependent terms vanished. This procedure was called "coiffuring". However, we find that, with the solutions generated with the new solution-generating technique, the right-hand sides of the second-layer equations are automatically v-independent. For this reason, we assume that all b k,m,n 1 are also vanishing. In this case the only non-trivial source in the second-layer equations is Θ 4 ∧Θ 4 which takes the simple form written on the right-hand side of (6.4). Since there are no potentially dangerous terms to be taken care of by coiffuring,

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the ansatz we use for the first-layer solution of a single-mode superstrata is simply We now want to solve the second-layer equations where the source on the right-hand side is determined by (6.2). By following [25] we take the following ansatz for F and ω where ω 0 is given in (3.10), and the RMS superscript denotes that the ansatz functions are independent of the coordinate v and are thus non-oscillating. We assume that F RMS and the components of ω RMS only depend on the coordinates r and θ and that ω RMS r = ω RMS θ = 0. Using (6.2) on the right-hand side of the second-layer equations, we see that the RMS parts of (6.3) are governed by the differential equations where we have used the fact that d 4 ω 0 is anti-self-dual and have introduced L ≡ − * 4 d 4 * 4 d 4 as the Laplace operator in the four-dimensional Euclidean base space. Notice that the top differential equation has a vanishing right-hand side, which was not the case in previously known examples. One can show that when acting on a scalar function that depends only on r and θ, the Laplace operator can be written as

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Notice that (6.4b) is already in the form (6.6), and can be thus solved by a linear combination of the F functions.
To get the solution for ω, we introduce the ansatz 21 [25] ω RMS = µ k,m,n (dψ + dφ) + ν k,m,n (dψ − dφ) , (6.9) and define a new function µ k,m,n ≡ µ k,m,n + R y 4 √ 2 where F k,m,n ≡ F is the solution of (6.4b). One can show that µ k,m,n satisfies the differential equation which can be again solved by a linear combination of the functions (6.7). One is thus able to determine F k,m,n and µ k,m,n as the solution of their respective second-order differential equations. By following the same approach of [25], one can show that the explicit forms of the ansatz quantities are given by where in (6.12b) we have added an additional harmonic piece that is left undetermined by the differential equations. Its form is chosen so that the solution is regular at the centre of the coordinate system and will be determined in the next subsection. The remaining ν k,m,n functions are obtained by solving first-order differential equations, which contain F k,m,n and µ k,m,n as sources. These equations are ∂ r ν k,m,n = − a 2 + r 2 sin 2 θ − r 2 cos 2 θ r 2 + a 2 sin 2 θ ∂ r µ k,m,n − 2r sin θ cos θ r 2 + a 2 sin 2 θ ∂ θ µ k,m,n − √ 2a 2 R y a 2 + 2r 2 r sin 2 θ cos 2 θ r 2 + a 2 sin 2 θ Σ 2 F k,m,n , (6.13a) ∂ θ ν k,m,n = 2 a 2 + r 2 r sin θ cos θ r 2 + a 2 sin 2 θ ∂ r µ k,m,n + r 2 cos 2 θ − a 2 + r 2 sin 2 θ r 2 + a 2 sin 2 θ ∂ θ µ k,m,n + √ 2a 2 R y a 2 + r 2 r 2 sin θ cos θ cos 2θ r 2 + a 2 sin 2 θ Σ 2 F k,m,n . (6.13b) These equations can be solved by integration on a case-by-case basis for each set of quantum numbers.

Regularity
We want our solutions to be free of any singularities. However, the coordinates introduced in (3.9), which are used to describe the solutions, have points at which they degenerate. Hence using these coordinates we have to take special care of the functions and components of the forms in order for our solutions to be regular. There are regions of the base manifold at which the coordinates degenerate. The first one is at θ = 0, where the φ circle degenerates. The second one is at θ = π 2 , where the ψ circle shrinks. Finally at the locus (r = 0, θ = 0) the entire sphere S 3 θφψ shrinks. Imposing regularity at these regions imposes constraints on our solutions. We will look at each of the constraints separately. Since now the scalar functions Z 1 and Z 2 are the same as the seed solutions and Z 4 is vanishing, we only focus on the regularity of the forms. The standard procedure to check the regularity is to express the forms in a coordinate system without any degenerate points. However, we will instead impose the equivalent condition that form components along dφ and dψ vanish at a degenerate locus.
We start by looking at the region where (r = 0, θ = 0). Focus on the regularity of the 1-form ω, especially on the dψ + dφ component, which explicit expression is given in (6.12b). In order to cancel out the singularity caused by the form legs, µ k,m,n needs to vanish at the point of interest. This determines the constant multiplying the harmonic term in µ k,m,n , which must be (6.14) Again the x notation is used to distinguish the normalisation from the q = 0 case. The same analysis needs to be repeated for the dψ − dφ component of the one-form, which also needs to be vanishing at the centre of the base manifold. However, as we are currently lacking a closed expression for generic quantum numbers, the analysis needs to be done on a case-by-case basis. Let us now look at the points of the location of the supertube, namely (θ = π 2 ). This is the same as looking at Σ = 0, where the scalars Z 1 and Z 2 diverge. To check the regularity of the solution, we look at the (dφ + dψ) 2 component of the metric and demand that it is regular at the position of the supertube. Imposing regularity at this locus of spacetime changes the relation between the brane charges Q 1 , Q 5 and the parameters defining the supertube ansatz a and b, which is now given by where x k,m,n is defined in (6.14).

Asymptotically flat solution
Up to this point, the solutions we presented are asymptotically AdS 3 × S 3 × T 4 , which allows for the identification with the dual CFT states discussed in section 2. It turns out that these solutions can be extended to asymptotically flat configurations (in our case that

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is asymptotically equal to R 4,1 × S 1 × T 4 ) in a straightforward way and so can be identified with microstates of asymptotically flat black holes. As usual, this is done by adding back "1" in the functions Z 1 and Z 2 . By introducing this extra constant, one usually obtains additional v-dependence on the right-hand side of second-layer equations. The effect of these additional terms is that we get new v-dependent terms in (6.3), with the differential equations determining these new terms usually being cumbersome to solve. Luckily, the novel feature of the solution (6.2) is that including the constant term in Z 1,2 does not add any additional source terms into the second-layer equations. Thus focusing on the single-mode superstrata, the asymptotically flat extension of the solution (6.2), gives the same second-layer equations for F and ω as in the asymptotically AdS case. So, both the asymptotically AdS and the full asymptotically flat solution are v-independent.

Conserved charges
One can extract the conserved charges of our new solutions from their large-distance behaviour. This gives a consistency check of the proposed identification between the new superstrata and the CFT states (2.10). The angular momentum charges J and J associated with the left-moving and rightmoving sector of the CFT respectively are related to the J φ and J ψ components of the supergravity angular momentum through These charges can be found by analysing the g φψ component of the ten-dimensional metric. In our ansatz, this component is obtained by looking at the φ + ψ components of the oneforms β and ω. It is straightforward to adapt the general prescription of [61] to this case (see for instance [48]), and one obtains Thus it is possible to read off the angular momenta of our newly obtained solutions from the knowledge of β (which is unchanged from (3.10a)) and µ (6.12b). One finds that these are given by Similarly, the momentum charge Q p can be extracted from the large-distance behaviour of the function F:

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For our new solutions, we find x k,m,n . (6.21) Finally, we note that the brane charges Q 1 and Q 5 that appear in the scalar functions Z 1 and Z 2 do not change, as the two functions remain unchanged from the seed solutions (3.10).
The supergravity charges calculated above are proportional to the quantised charges calculated on the CFT side. The brane charges Q 1 and Q 5 are related to the D-brane numbers n 1 and n 5 through with V 4 being the coordinate volume of T 4 , g s the string coupling, and α ′ the Regge slope. The relation between the Q p obtained in (6.20) and the quantised momentum number n p is The angular momenta J,J obtained from the supergravity calculation in (6.18) are related to the quantised ones j,j by We are now able to compare the charges obtained from the supergravity solutions with the ones calculated on the CFT side. The latter are given by (2.11). The crucial point at this step is to identify the supergravity constraint obtained from the regularity condition at the position of the supertube (6.15) and the CFT constraint for the total number of strands (2.10). The parameter a is connected with the number of untwisted strands N a and the number of twisted strands N b with the parameter b. We find that these quantities are connected by Using this identification together with the relations between the supergravity and quantised momenta, we get that the CFT charges corresponding to the supergravity solutions obtained above are given by 22

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for the angular momenta, and using that the momentum charge n p = h R −h R , we get We see that in all three cases these charges agree with the ones given in (2.11), if we set q = 1, as we should for our new supergravity solutions. This provides a check that the newly obtained solutions really are dual to the CFT states (2.6), with q = 1.

Compendium of formulas and explicit solutions
Here we collect the expressions for the new superstrata that we constructed in this paper.
The new superstrata represent supersymmetric solutions of supergravity, whose 10dimensional fields are given by the ansatz (3.1). The quantities that enter the ansatz satisfy two layers of BPS equations, which are differential equations on a four-dimensional base, which we took to be flat R 4 . The ansatz quantities that solve the first-layer equations (3.5) are where the definitions of ∆ k,m,n andv k,m,n can be found in (3.18) and the self-dual twoforms Ω (i) are given in (3.19). The range of the integers (k, m, n) is Due to the linearity the BPS equations, an arbitrary superposition of solutions (7.1) is still a solution of the first-layer equations (see (6.1)). However, in this paper, we limited ourselves to single-mode superstrata, for which only one of the coefficients b k,m,n 4 ≡ b is nonvanishing. In this case, the ansatz quantites that solve the second-layer BPS equations (3.8) are given by F = F RMS (r, θ), ω = ω 0 + ω RMS (r, θ) , where ω 0 is defined in (3.10c), ω RMS = µ k,m,n (dψ + dφ) + ν k,m,n (dψ − dφ) , (7.3) and while ν k,m,n has to be calculated on a case-by-case basis using the differential equations (6.13). The functions F 2k,2m,2n are given by (6.7) and the coefficient x k,m,n is fixed by regularity of the solution to be (6.14).

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In the dual CFT, the single-mode superstrata correspond to states of the form where |k, m, n, q R is the spectral flow to the R sector of the NS state |k, m, n, with q = 0, 1. States with q = 1 are dual to the new superstrata while the states with q = 0 are dual to the original superstrata constructed in [25]. The relation between the supergravity parameters a, b and the CFT parameters N a , N b is given by (7.5).
The above solutions are asymptotically AdS 3 but by simply setting the solutions become asymptotically flat. Such a transformation does not spoil the secondlayer equations, meaning that the F k,m,n and ω k,m,n are still valid solutions, even in the asymptotically flat case. In contrast, extending the original superstrata to asymptotically flat ones required a non-trivial step of solving differential equations [25].

Explicit examples
The solutions above are valid for any allowed set of quantum numbers (k, m, n, q = 1). However, F k,m,n and µ k,m,n contain linear combinations of F 2k,2m,2n , which include nontrivial sums and are generically hard to evaluate. However, in certain cases, these sums can be evaluated explicitly, which then makes it possible to find solutions to the second-layer BPS equations in a closed form. Here we present the explicit expression for F k,m,n , ω k,m,n for two classes of solutions.
7.1.1 (k, m, n, q) = (k, 0, 0, 1) class of solutions The simplest class of solutions is parametrised by the quantum numbers (k, m, n, q) = (k, 0, 0, 1), with k being an arbitrary positive integer. These geometries already carry three charges, as momentum is added through the action of the fermionic generators. They are given by ψ (X; k) Z 2 cos 2 θ dψ , (7.8b) where we introduced the notation X = a 2 sin 2 θ r 2 + a 2 , Z = r 2 r 2 + a 2 , φ denote polynomial functions in the variable X with the parameter k. They are given by The above gives regular solutions for any k > 1.
It is interesting to see what happens for k = 1. If we treat k as a continuous parameter, one can notice that all functions P in (7.10) vanish linearly as k → 1, and so F k,0,0 and ω k,0,0 have a simple pole at this value of k. This means that the solution is ill-defined for k = 1, which is consistent with the CFT result in section 2 that the states |1, 0, n, 1 NS are unphysical. One may think that one could multiply b 2 by (k − 1) to start with in order to cancel this pole and get a physical solution. However, one can show that the solution with such modified normalisation would contain a logarithmic divergence at θ → 0 and does not represent a phyically allowed geometry. 7.1.2 (k, m, n, q) = (2, 0, n, 1) class of solutions The next simplest, physically meaningful class of three-charge examples is given by the quantum numbers (k, m, n, q) = (2, 0, n, 1), where n = 0, 1, 2, . . .. In the case where n = 0 the momentum charge is coming purely from fermionic generators, whereas for n = 0 the momentum charge is also added through the action of bosonic generators. One finds that

Acknowledgments
We thank Stefano Giusto for useful discussions. This work is supported in part by the

A Conventions
Most of the conventions used in this paper follow directly the conventions used in [40]. 23 Here we present only a brief summary of the most important conventions used throughout the main text.

A.1 Supersymmetry variations
From [57, (2.17)], the supersymmetry transformations for bosonic fields in type IIB supergravity are given by 23 See appendix A of that paper.

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where µ, ν, . . . are curved spacetime indices while a, b, . . . are local Lorentz indices. The fermionic field variations read where n = 1/2, . . . , 9/2 and P = −σ 3 , P n = σ 1 n + 1/2: even acts on the doublet index of the gravitino ψ 1,2 µ and dilatino fields λ 1,2 , which was suppressed in the expressions above. We have also introduced the slashed notation where every form index is contracted with a gamma matrix. The RR field strengths are related to the RR potentials by Using the Γ-matrix algebra and the self-duality relations of the RR field strengths, one can write the variations (A.2) explicitly as where ∇ M = ∂ M + 1 4 ω M ab Γ ab with ω M the spin connection 1-form. In deriving the above relations, we also used the fact that ǫ 1,2 are Majorana-Weyl spinors with positive chirality.

A.2 Spinor conventions
In the above we mentioned that the supersymmetry variations are generated by Majorana-Weyl spinors. The 10-dimensional Weyl condition is given in (4.13). If we take the charge conjugation matrix C to be C = Γ t , (A.8)

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simply means that the spinor is real, ǫ * = ǫ. (A.10) Note that for a Majorana spinor one hasǭ In most of our analysis we use the coordinates u and v defined in (3.3). It is convenient to express Γ t as where Γ u and Γ v are defined in (4.12). They are convenient to work with, when acted upon a spinor with a definite eigenvalue under Γ uv . They satisfy where we used the hermiticity properties of the Γ matrices, (A.14) As an example, using all these conventions, we find that the transpose of the spinor (5.1) used to generate the double variation (5.4) is given by

A.3 Identifying Killing spinors and CFT fermionic generators
Here we will give justification for the identification (4.18), (4.19) between the components of the Killing spinors ζ ± and the CFT fermionic generators G αA As we can see from (4.10) and (4.11), the spinors ζ ± and ζ ± are related to the u-and v-dependent part of the Killing spinors, respectively. So, they are naturally linked with the left-moving (G) and right-moving ( G) sectors of CFT. Therefore, we will henceforth focus on the identification in the left-moving sector between ζ ± and G αA ± 1 2 . From the v-dependence in (4.11d), we have the tentative identification (A.16) The next issue is to relate the SU(2) L × SU(2) R R-symmetry on the CFT side and the SO(4) ∼ = SU(2) L × SU(2) R symmetry of the sphere S 3 on the supergravity side. It is clear that these symmetry groups are to be identified with each other but we would like to "align" them by identifying the "J 3 " generators on the two sides.
On the supergravity side, we can write down a set of SU(2) L × SU(2) R generators acting on spinors as

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or, more explicitly, These matrices satisfy the commutation relations and have Casimir operators given by (A.20) We turn our focus to the action of these matrices on the spinors ζ ± . Recall that these spinors must satisfy the conditions (4.13) and (4.16). Combining these two implies that they must satisfy Γ uvrθ φ ψ ζ ± = ζ ± . (A.21) From this condition together with (4.17), we find that From the Casimir operators (A.20), we conclude that ζ ± transform in the (2, 1) representation under the SU(2) L × SU(2) R generated by J a , J a . This is as expected, because ζ ± is to be identified with G αA ± 1 2 which transform in the same representation under the R-symmetry.
We need to identify which of the operators in (A.17) corresponds to the "J 3 " operator of the SU(2) L algebra on the CFT side. This operator will allow us to distinguish between the spinor components corresponding to G +A . In order to see that, we look at the spinor (4.10). By setting ζ ± = 0, we obtain a spinor with terms that contain the combination Y + ζ ± . Using the constraint (A.22) one can show that the combination appearing in the spinor can be rewritten as where P ± S is the projection operator onto the J ψ = ± 1 2 eigenspace defined in (4.18). Because the algebra (2.1) says that {G ±A 0 , a double variation by ζ ± should reproduce the bosonic symmetry J ± 0 whose realisation is given in (3.15). Since J ± 0 include a prefactor of e ±i( φ+ ψ) , we conclude that the J ψ = ± 1 2 eigenspaces, multiplied by e ±i φ+ ψ 2 in (A.23), are precisely the J 3 = ± 1 2 eigenspaces. Namely, J ψ can be identified with J 3 0 on the CFT side. This leads to a finer identification One can repeat the procedure for the SU(2) B × SU(2) C symmetry on the CFT side, which is to be identified with the symmetry of the internal T 4 on the supergravity side.

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We can write down a set of supergravity generators of SU(2) B × SU(2) C in the spinor representation as follows: which again satisfy the commutation relations and have Casimir operators Since our spinors satisfy the condition (4.16), we see that ζ ± both transform in the (2, 1) representation under SU(2) B × SU(2) C generated by B i , C i . This is accordance with the fact that G αA However, unlike the case of SU(2) L × SU(2) R , there is no unique way to align the SU(2) B × SU(2) C groups between supergravity and CFT, because our ansatz (3.1) does not distinguish the four directions inside the internal T 4 . As a result, in the Killing spinors (4.10), no Γ matrix with legs in the T 4 appear, and all Γ k with k = 6, 7, 8, 9 are on an equal footing. Therefore, we can choose the "J 3 " direction of SU(2) B as we like. Specifically, we define the projectors P A T , A = 1, 2 by (4.18) and identify its A index with the A index of G αA . This leads to the final identification which is (4.19) in the main text.

B Explicit results in the NS-NS sector
In section 4 we have calculated the variations of the dilatino fields generated by the AdS 3 × S 3 × T 4 Killing spinor ζ αA − . In a similar manner one can calculate the variations of the components of the gravitino fields. These are presented in this appendix and one finds some subtleties one does not find in the dilatino variation. Furthermore, we also give the variation of the fermionic fields generated by the spinor ζ αA + . We expect that these variations vanish, and in fact the dilatino variations do, but the gravitino component variations show the same subtleties as one finds in the variations of generated by the ζ αA − spinors. Finally we will present the results of the double variations of the components of the B-field in the NS-NS coordinates, which we omitted in the main text.

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B.1 Gravitino variations generated by ζ αA − One finds that the variations of the components of the gravitino field generated by the spinor (5.1) are given by 7, 8, 9, (B.1g) where Note that, for the variations generated by spinor (5.1), we have δψ 1 M,b = δψ 2 M,b for all M . We find that the gravitino variations (B.1) generically have two parts. The first one is analogous to the dilatino variation, as it contains the combination (cos θΓ rθ − iΓ r φ + sin θ), which when acting on the combination (Y + ζ αA − ) projects out the ζ −A − components of the spinor. This part is again expected from the fact that the perturbed geometry is dual to an anti-chiral primary state. The second part of the variations (given in the second lines of the respective variations) does not distinguish between the ζ +A − and ζ −A − components of the JHEP03(2019)095 spinors. We believe that these extra factors are related to the residual gauge freedom that we have in our system and one should be able to consistently ignore these extra factors. This claim is further strengthened by the fact that once we use these fermionic variations to calculate the double variations of bosonic fields, these additional terms consistently cancel out and thus do not contribute to any observable fields.

+
The claim that the extra terms found in (B.1) can be set to zero by gauge transformation is further supported by calculating the variations of fermionic fields generated by the Killing spinor components ζ αA + . Since these are dual to the modes G αA , the variations should vanish. Furthermore, one should not obtain any terms that would distinguish between the ζ +A + and ζ −A + components as now variations generated by both should vanish. If we set ζ αA − = 0 and make ζ αA + arbitrary, the spinor that generates the variation is given by Using this spinor as the generator of the solutions, one obtains that the explicit variations of the fermionic fields are given by and We see that the variations of the dilatino fields vanish, as expected. On the other hand, the variations of the components of the gravitino fields do not vanish. However, note that these variations only contain the terms which we deemed as a

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consequence of the gauge freedom in our system and lacks the term which would distinguish between the two SU(2) L components. Since these variations should be trivial, we get another confirmation that these terms appearing in the gravitino variations are not physical.

B.3 Variations of the B-field
The non-vanishing term in the double B-field variation is given by where in the last term we again used the fact that the only non-zero spinor components used to generate the variations are ζ +A − . The variations of the individual components of the B-field in the NS-NS sector are then given by where C Supergravity spectrum around AdS 3 × S 3 In the main text, we explicitly constructed a new 3-charge supergravity solution that corresponds to the CFT state (2.6) (or (2.10)). Surprisingly, at linear order, the supergravity solution only involved excitation of Θ 4 , which is related to the NS-NS B-field, and not any

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other fields such as Z 4 or the 4D base metric (even at the non-linear level, the only excited fields are Θ 4 , F, ω). Actually, this fact can be deduced from the analysis of the spectrum of 6D supergravity compactified on AdS 3 × S 3 , as we will discuss in this appendix. The spectrum of 6D supergravity compactified on AdS 3 × S 3 , which is relevant for the AdS 3 /CFT 2 correspondence, has been extensively studied [42][43][44][45] (see also [27]). Particularly useful for us is ref. [42] which, for D = 6, N = (2, 0) supergravity with n tensor multiplets, worked out the excitation spectrum around the AdS 3 /CFT 2 background and its explicit supermultiplet structure. Type IIB supergravity compactified on K3 corresponds to n = 21, for which the theory is anomaly free. On the other hand, T 4 compactification can be studied by taking n = 5, although this truncates fields that correspond to gravitino multiplets of the N = (2, 0) theory (see ref. [44] which studied the spectrum in the T 4 case including the gravitino multiplets).
Here we briefly summarise the result of ref. [42] and relate it to our setup. Note that our convention for the R-charge is opposite to that in [42]; so, chiral primaries there correspond to anti-chiral primaries in our setup, and G ±A n , G± A n there correspond to G ∓A n , G∓ A n in our setup.
The D = 6, N = (2, 0) supergravity theory has the duality group SO(5, n), and its bosonic fields are the graviton g M N , 5 2-form potentials B i M N with self-dual field strengths, n 2-form potentials B r M N with anti-self-dual field strengths, and 5n scalars. Here, M, N, . . . are curved 6D indices, i = 1, . . . , 5 is the SO(5) vector index, and r = 6, . . . , 5 + n is the SO(n) vector index. The scalars live in the coset space SO(5, n)/(SO(5) × SO(n)) and can be parametrised by vielbeins (V i I , V r I ) where I = (i, r) = 1, . . . , 5 + n is the SO(5, n) vector index. Self-duality (anti-self-duality) is not imposed on the 3-forms G i = dB i and G r = dB r but on H i = G I V i I and H r = G I V r I ; namely, they satisfy * 6 H i = H i and * 6 H r = −H r . Small fluctuations around the AdS 3 × S 3 background can be studied by writing the fields as g M N =ḡ M N + h M N , G I M N P =Ḡ I M N P + g I M N P , V i I = δ i I + φ ir δ r I , V r I = δ r I + φ ir δ i I . (C.1) Here,ḡ M N is the background AdS 3 × S 3 metric andḠ I M N P is the background 3-form field strength with components where m −1 is the radius of AdS 3 × S 3 , µ, ν, . . . are curved AdS 3 indices, and a, b, . . . are curved S 3 indices. To support the AdS 3 × S 3 background, we must turn on one of the self-dual form fields, which we have taken to be the i = 5 one. This breaks the SO (5) R-symmetry of 6D supergravity to SO(4). 24 We use i = 1, . . . , 4 for the vector index for this unbroken SO(4). This SO(4) = SU(2) B × SU(2) C symmetry is not to be confused with the SO(4) = SU(2) L × SU(2) R R-symmetry of the CFT coming from the isometry of the S 3 . Rather, SU(2) B is related to the SU(2) outer automorphism of the N = (4, 4) superconformal algebra, while SU(2) C is related to a custodial symmetry with respect which the fundamental fields of the CFT are charged (but not the superconformal generators are).

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We can relate the above fields in 6D supergravity to the quantities appearing in the main text as follows. First, the self-dual H i=5 and the anti-self-dual H r=6 are related to the self-dual and anti-self-dual linear combinations of the RR 3-form F 3 and its 6-dimensional dual * 6 F 3 [27], while the scalar φ 56 is related to the dilaton which is roughly Z 1 /Z 2 . To discuss r = 7, . . . , 5+n, let us recall that there are (n−1) (1, 1)-forms in T 4 (n−1 = 4) and K3 (n − 1 = 20). Among them is the Kähler form J ≡ ω (7) . Let us denote the remaining (n − 2) (1, 1)-forms by ω (r) , r = 8, . . . , 5 + n. The relations are slightly different for r = 7 and r ≥ 8. The 3-form H r=7 is related to the NS-NS 3-form H 3 which in turn is related to the 2-form Θ 4 , and the scalar φ 57 is related to Z 4 . On the other hand, H r=8,...,5+n are related to the part of the RR 5-form F 5 involving ω (r) , and the scalar φ 5r is related to the part of H 3 involving ω (r) [62].
The fields h M N , g I M N P , and φ ir represent small fluctuations around the background and can be decomposed as (C.4) In the de Donder-Lorentz gauge, the fluctuation fields can be expanded in the harmonic functions in S 3 as The SO(4) quantum numbers ℓ 1 , ℓ 2 of the S 3 harmonic functions Y (ℓ 1 ,ℓ 2 ) (s) are related to the SU(2) L × SU(2) R quantum numbers j,j in the main text as The subscript (s) denotes the SO(3) content associated with the tangent space of S 3 . By substituting the above expansion into the field equations of the D = 6 supergravity, one obtains the spectrum of excitations and their representation content. The SO (2,2) representation associated with the AdS 3 can be labeled by the energy E 0 and the spin s 0 , which are related to the weights h,h in the main text as Table 1. The fields excited in various superdescendant states. The fields in each row are described by a coupled system of equations which must be diagonalised to find the spectrum [42]. The shorthand GG means G +1 −1/2 G +2 −1/2 , G G means G+ 1 −1/2 G+ 2 −1/2 , and G G means the four combinations G +A −1/2 G+ B −1/2 with A, B = 1, 2. The states in (red) boldface letters are supersymmetric, involving only G and not G. The meaning of the prime on |++ ′ and |−− ′ is explained in the main text.
This procedure was carried out in [42], where they have explicitly written down which fields are involved in each excitation mode. Furthermore, by examining the quantum numbers of the supercharges associated with the Killing vectors of the AdS 3 × S 3 background, they identified the supermultiplets that these excitation modes are the members of. By comparing the representation content of these supergravity supermultiplets with the representation content of the CFT supermultiplets obtained by acting with G +A −1/2 and G+ A −1/2 on the anti-chiral primaries 25 |±± k , |±∓ k and |00 k , we can find what fields are excited in the supergravity modes dual to each such state. In table 1, we listed the fields are excited for anti-chiral primary and superdescendant states (cf. table 1 of [42]).
The anti-chiral primary state |00 k in table 1 does not only mean the one considered in the main text but represents a set of n − 1 states corresponding to the (1, 1)-forms ω (r) , where r = 7, . . . , 5 + n. In order to furnish a complete vector representation of the SO(n) symmetry that exists in supergravity, we need to add one extra state to the above n − 1 states. The candidate anti-chiral primaries are |++ k+1 and |−− k−1 , which have the same charges as |00 k (h = −j 3 = k 2 ). Because the supergravity modes that correspond to |00 k leave the 6D metric unchanged, the extra state must also leave the 6D metric unchanged. Indeed, there is a linear combination of |++ k+1 and |−− k−1 whose gravity dual has undeformed 6D metric at linear order; see footnote 9 of [63]. 26 Let us JHEP03(2019)095 denote by |++ ′ k such a linear combination. Then the vector of SO(n) is given by the n-vector (|++ ′ k+1 , |00 k ). We also define |−− ′ k to be the linear combination of |++ k+1 and |−− k−1 that is orthogonal to |++ ′ k . Using the relation between the 6D supergravity in table 1 and the fields discussed in the main text, we can figure out what fields (such as Z 4 and Θ 4 ) are excited for what superdescendants. From the second last line of table 1, we see that the supergravity mode corresponding to the CFT state G +1 |00 , which has been the focus of the current paper, only involves Z r µ . This is related to the mixed component (between AdS 3 and S 3 ) of the anti-self-dual 2-form B r M N . In particular, it does not change the 6D metric at the linear order. This means that this mode only excites Θ 4 but none of Z 1,2,4 , which is what we found in the main text.
It is interesting to see that there are other supersymmetric modes that excite only one field. First, we see that the state G +1 |++ ′ do not excite the metric. The nonlinear completion of this would be the GG version of the "Style 1" superstratum discussed in [64]. Moreover, the state G +1 |+− turns only on L, which is related to the traceless part of the S 3 metric. This will probably correspond to some simple deformation of the 4D base metric with β unchanged. It would be interesting to construct the non-linear completion of these modes. Although it must be technically more challenging, some of nonsupersymmetric states, namely G G|00 , G G|++ ′ , G G|∓± , have only one field excited, and constructing their non-linear completion would be also interesting. See [65] for recent work in this direction.

D Killing spinors in the RR coordinates
In the main text, we studied the Killing spinors of AdS 3 × S 3 in the NS-NS coordinates. Here we derive the expression for the Killing spinor in the RR coordinates and further show that the two sets of spinors are related by a local Lorentz transformation and the spectral flow coordinate transformation.
We summarise some formulas that we make frequent use of in this appendix.

Map between the NS-NS and RR spinors
In the above, we derived the expression for the Killing spinors in the RR coordinates with the vielbeins (D.5). On the other hand, in the main text, we derived the Killing spinors in the NS-NS coordinate system with the vielbeins (4.6). The two Killing spinors are related by a coordinate transformation and a local Lorentz transformation, which we work out below. The vielbeins used in the NS-NS coordinates are: E v = 1 2 aR y r 2 + a 2 + r dv + r 2 + a 2 − r du , E u = 1 2 aR y r 2 + a 2 + r du + r 2 + a 2 − r dv , E φ = aR y sin θ d φ, E ψ = aR y r cos θ d ψ, (D. 16) where we put tildes on the NS-NS vielbeins, to distinguish them from the RR ones (D.5).
The components E r , E θ , E α are the same as the RR ones and we did not write them down. The RR angles (φ, ψ) and the NS-NS ones ( φ, ψ) are related to each other by the spectral flow transformation (3.12).
The two sets of vielbeins are related by a local Lorentz transformation and the coordinate transformation (3.12). Let us focus only on the (u, v, φ, ψ) and (u, v, φ, ψ) parts of the vielbeins because other parts are identical in RR and NS-NS coordinates. Then the Lorentz transformation can be written as where Λ = Λ 5 Λ 6 Λ 3 Λ 4 Λ 1 Λ 2 , Λ i = e a i g i . (D. 18) Here g i are given by g 1 = iM uv , g 2 = −iM φψ , g 3 = iM uφ , g 4 = iM uψ , g 5 = iM vφ , g 6 = iM vψ (D. 19) with M ab the Lorentz generators in the vector representation given by The parameters a i are given by a 1 = log aR y √ r 2 + a 2 + r 2Σ , a 2 = θ − γ, a 3 = − ar sin θ √ 2 Σ , a 4 = a √ r 2 + a 2 cos θ √ 2 Σ , a 5 = − √ 2 a sin θ √ r 2 + a 2 + r , a 6 = − √ 2 a cos θ √ r 2 + a 2 + r . (D.23) Spinors transform as scalars under coordinate transformation and transform in the spinor representation under local Lorentz transformation. Therefore, if we act on the RR spinor ǫ R − with the matrix Λ in the spinor representation and replace explicit φ, ψ appearing in ǫ R − by φ, ψ using (3.12), we must get the NS-NS spinor ǫ NS − . Here, we put "R" and "NS" on ǫ − to clarify the frame that the spinor is in. Namely, ǫ NS = Λ spinor ǫ R . (D.24) The local Lorentz generators in the spinor representation are given by 25) or, more explicitly, (D. 26) In doing this, we must note that we do not transform the matrices Γ µ ; they are always constant matrices and the index µ is only a label. Therefore, Γ φ , Γ ψ are the same constant matrices as Γ φ , Γ ψ . Let us explicitly prove the relation (D.24). For simplicity, we consider ǫ − in the R sector, (D.7), in the case with χ + = 0. In this case,  Because Γ v , Γ u square to zero, we find Γ uψ e γΓ φψ , (D.31) (D.34c) In order to match two expressions, let us decompose χ − into the representation of the SU(2) L × SU(2) R symmetry group, whose generators are 28 where Ry ) χ −− . (D.39) 27 As explained below (D.26), the matrices Γ φ , Γ ψ are identical to the matrices Γ φ , Γ ψ . Therefore, Γ θ φ = Γ θφ , Γ r ψ = Γ rψ . 28 These are the same matrices as (A.18) (also see the comment below (D.26)).