Supersymmetric geometries of IIA supergravity II

We solve the Killing spinor equations of standard and massive IIA supergravities for a Killing spinor whose isotropy subgroup in Spin(9, 1) is SU(4) and identify the geometry of the spacetime. We demonstrate that the Killing spinor equations impose some mild constraints on the geometry of the spacetime which include the existence of a time-like Killing vector field which leaves the fields and the Killing spinor invariant.


Introduction
The systematic investigation of the supersymmetric backgrounds of standard [1]- [3] and massive [4] IIA supergravity has been initiated in [5] where the maximally supersymmetric backgrounds have been classified. Furthermore, in [6] it has been shown, following a similar result for IIB supergravity in [7], that all backgrounds preserving 31 supersymmetries are maximally supersymmetric. More recently, it has been found in [8], using spinorial geometry [9], that there are four different types of massive (IIA) backgrounds preserving one supersymmetry each associated to one of the four types of non-trivial orbits of the spin group Spin(9, 1) on the 32-dimensional Majorana spinor representation. Furthermore, the geometry of backgrounds associated to orbits with isotropy groups Spin (7) and Spin(7)⋉R 8 has been described [8].
The main purpose of this paper is to present the geometry of (massive) IIA backgrounds preserving one supersymmetry which are associated to the orbit with isotropy group SU (4). The geometry of the backgrounds whose Killing spinor represents the remaining orbit, whose isotropy group is G 2 , will be presented elsewhere. A spinor representative of the orbit with isotropy group SU(4) is ǫ = f (1 + e 1234 ) + g 1 (e 5 + e 12345 ) + ig 2 (e 5 − e 12345 ) (1.1)

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where f , g 1 and g 2 are real constants with f = 0, g 2 = 0, which later will be promoted to spacetime functions. Note that if g 2 = 0, then the isotropy group enhances to Spin (7). The spacetime of backgrounds preserving one supersymmetry does not necessarily undergo a reduction of its structure group. Typically, one expects that the Killing spinor will change orbit type from patch to patch. As the Killing spinor solves a parallel transport equation, it is no-where vanishing on the spacetime provided that the fields are smooth. However, the mere existence of a no-where vanishing section of the Spin bundle does not impose a topological restriction on the spacetime. In particular, the G-structure of the spacetime does not necessarily reduce. This is because the rank of the Spin bundle is much larger than the spacetime dimension and so no-where zero sections are allowed. Nevertheless, the spinors with the four different isotropy groups describe locally all possible geometries of backgrounds preserving one supersymmetry. Furthermore, there are backgrounds for which the Killing spinor does not change orbit type. The structure group of such backgrounds reduces to a subgroup of the stability group of the corresponding orbit.
Having identified a representative spinor of the SU(4) orbit that we shall investigate, we apply spinorial geometry [9] to turn the Killing spinor equations (KSEs) into a linear system for components of the fluxes and the spin connection. In this case, all these components are automatically expressed in representations of SU (4). The solution of the linear system reveals the conditions on the geometry implied by the existence of a Killing spinor as well as an expression for the fluxes in terms of the geometry. The conditions on the geometry, given in (2.3), (2.6), (2.7) and (2.8), for the existence of a Killing spinor with isotropy group SU(4) are rather mild. In particular, it is required that the spacetime admits a time-like Killing vector field which leaves all the fluxes invariant as well as the Killing spinor itself. In particular, the latter condition implies that the spinorial Lie derivative of the Killing spinor along the time-like Killing vector bilinear vanishes. The two additional conditions will be described later.
The expression of the fluxes in terms of the geometry is not particularly illuminating. This is in contrast to the Spin(7) and Spin(7) ⋉ R cases in [8] for which the expressions are rather simple. Because of this, we do not solve the linear system for the fluxes completely. Nevertheless the vast majority of the fluxes are expressed in terms of the geometry and it is only a few equations that are maintained in their linear system form.
Apart from the generic SU(4) backgrounds described above, there is a special class of SU(4) backgrounds for which g 1 = 0. This special class of backgrounds is not an artefact of the gauge used to put the Killing spinor in the form (1.1) as these backgrounds can also be characterised by the vanishing of a scalar bilinear. The linear system in this special class of SU(4) models undergoes a dramatic simplification reminiscent that of the IIB backgrounds associated with a pure spinor. The conditions on the geometry are the same as those of the generic backgrounds above. Now however, the expression of the fluxes in terms of geometry is much simpler. We shall exploit this fact to completely solve the linear system and express the fluxes in terms of the geometry. This paper has been organised as follows. In section two, we explain the solution of the KSEs for generic SU(4) backgrounds and describe the geometry of spacetime. In section three, we present the solution of the KSEs for the special class of SU(4) backgrounds with JHEP12(2015)113 g 1 = 0. In appendix A, we describe our conventions and give some useful formulae. In appendix B, we give the spinor form bilinears of the SU(4) invariant spinors. In appendix C, we present the linear system for a generic SU(4) invariant Killing spinor, and in appendix D we give the solution of the linear system for the special case g 1 = 0.

Solution of the KSEs for generic SU(4) backgrounds
To solve the KSEs of (massive) IIA supergravity we promote f, g 1 and g 2 to real spacetime functions and substitute the spinor ǫ in (1.1) into the KSEs. 1,2 We assume that f, g 2 do not vanish while g 1 may vanish at some points but otherwise it is generically non-zero. Then we apply the spinorial geometric technique described in [9] to turn the KSEs into a linear system which contains components of the fluxes and of the spin connection as variables. All these components are naturally expressed in SU(4) representations and so no further work is required to re-express the linear system in terms of the representations of the isotropy group of the Killing spinor. Then, the linear system is solved by expressing some of the components of the fluxes in terms of the spin connection. In addition, the linear system imposes some conditions on the geometry of the spacetime. In the context of spinorial geometry these appear as linear equations which involve only the components of the spin connection as well as the functions f, g 1 and g 2 and the dilaton Φ. Typically these geometric conditions can be re-expressed in many different ways; one such way involves the differentials of the fundamental forms of SU(4).
We do not present the linear system associated with the KSEs of (massive) IIA supergravity for the (1.1) spinor in its original form as this is derived from the application of spinorial geometry. Instead, we give a refined version which approaches the solution of the linear system in appendix C, and in what follows we shall explore the properties of this solution.

Geometry of spacetime
To describe the geometry of spacetime, first note that from spinorial geometry considerations there is a frame e A such the spacetime metric can be written as where ds 2 (8) = 2δ αβ e α eβ is a metric transverse to the lightcone directions e + and e − and α, β = 1, . . . , 4 are holomorphic SU(4) frame indices. Of course such a splitting is only on the tangent bundle of the spacetime and the metric potentially depends on all spacetime coordinates.
Next let us consider the form bilinears of the Killing spinor ǫ in (1.1). These are given in appendix B. Before we proceed observe that under a boost in the 5 direction, which is a gauge symmetry of the theory, f → ℓf while g 1 , g 2 → ℓ −1 g 1 , ℓ −1 g 2 . As a result, we can choose the gauge f 2 = g 2 1 + g 2 2 . In this gauge, one finds that the 1-form bilinears become after an additional trivial numerical normalization.
1 Throughout this paper we follow the conventions of [8] for the fields, spinors, KSEs and field equations. 2 To get standard (non-massive) IIA supergravity, put the mass parameter S = 0 in what follows.
In fact, this vector field leaves invariant all the other fields of the theory. This was expected as it is well known that this 1-form bilinear generates a symmetry of the theory [10][11][12].
In addition, the geometric conditions imply that This is significant even though X does not generate a symmetry for the backgrounds, as it is possible to adapt local independent coordinates for both K and X so that the expression for the fields can be simplified. For example, if K = ∂ τ and X = ∂ σ , the spacetime metric can be written as where m and n are 1-forms and ds 2 (8) is a metric in the directions transverse to X and K. All the components of the metric do not depend on τ but they can depend on σ and all the remaining coordinates of the spacetime.
Therefore, the Killing spinor ǫ is invariant under the motion generated by K.
The two conditions above provide a geometric description of all conditions imposed by the KSEs on the geometry of spacetime apart from (C.18) and (C.20). For the former one can show, after some calculation, that this condition can be expressed as Similarly, (C.20) can be written as This concludes the discussion of the geometry.

Fluxes in terms of geometry
The solution of the linear system also expresses some of the components of the fluxes in terms of the geometry. As these components are already in SU(4) representations, the solution of the linear system presented in appendix C is already in the required form.

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In particular denoting collectively the 2-form, 3-form and 4-form field strengths with G k , k = 2, 3, 4, we first decompose them as where the subscript in the brackets denotes the degree of the form in the directions transverse to e 0 and e 5 or equivalently e + and e − . Furthermore each component G k (8) representations. The resulting components are given in terms of the geometry as in appendix C. It may appear that the corresponding expressions are not covariant as they contain components of the spin connection. However this is not the case. All the components of the spin connection that appear in the expressions for the fluxes in appendix C actually transform as tensors under SU(4) gauge transformations. So provided that the spacetime has an SU(4) structure these expressions patch in a covariant manner on the spacetime manifold M .
For example the (1, 2) and traceless part of G 4 −(3) and G 4 +(3) are given in (C.62) and (C.63), respectively, in terms of the geometry and the (1,2) and traceless component of H 3 (3) . Note that this component of H 3 (3) is not restricted by the KSEs. In a similar way one can read the remaining equations in appendix C. However, solving the equations involving the P − and P + projections in appendix C, although possible, does not give an illuminating answer. As a result, we shall not attempt to give the full expression of the fluxes in terms of the geometry. The form already presented in appendix C is more economical.

Solution of the KSEs for a special case of SU(4) backgrounds
The special backgrounds that we shall be considering are those for which the scalar bilinear σ in appendix B vanishes. As f = 0, this condition implies that g 1 = 0. As the vanishing of a scalar is a covariant statement, it can be imposed globally on a manifold because it is consistent with the patching conditions. So this special class of backgrounds does not depend on the choice of representative for the spinor ǫ in (1.1).
These special IIA backgrounds are reminiscent of the IIB backgrounds in [13] which admit a pure spinor as Killing spinor. In particular, the linear system, as in the IIB case, simplifies considerably. This particularly applies in the gauge gḡ = f 2 that we shall use throughout. As a result f 2 = g 2 2 and so f = ±g 2 . In what follows we shall take f = g 2 ; the other case can be treated symmetrically.

Geometry of spacetime
The geometry of spacetime is as that described in the generic case after imposing g 1 = 0 on all geometric conditions in section 2.1. The only significant change is in equation (2.7) where now ∂ 5 log(g/ḡ) = 0.

Fluxes in terms of geometry
The expression of the fluxes in terms of the geometry is somewhat simpler in this case. The linear system can be solved and the solution has been presented in appendix D.
It can be seen from the solution that not all components of the fluxes are given in terms of the geometry. For example the traceless (1,1) component of G 4 +−(2) and the traceless (2,2) component of G 4 (4) are not given in terms of the geometry and so they are not constrained by the KSEs. The components of the fluxes that are given in terms of the geometry have been expressed in terms of components of the spin connection as well as in terms of components of the fluxes that are not constrained. There are various ways to reexpress these fluxes, for example in terms of the spinor form bilinears given in appendix B. For this one has to use the relation of these to the components of the spin connection as given in appendix A.

Acknowledgments
UG is supported by the Knut and Alice Wallenberg Foundation. GP is partially supported by the STFC grant ST/J002798/1.

A Conventions and useful SU(4) formulae
The conventions for the fields, KSEs and field equations of standard [1]- [3] and massive [4] IIA supergravity that we use are as those in [8] which have been adapted from the string frame formulation of the theory as in [14] and [15].
Our spinor conventions and in particular the null basis we use to express the spinor representative (1.1) of the SU(4) orbit are as in [9] and [16]. In these works, it is also explained how to realise the spinors in terms of forms.
The components of the spin connection that appear in the linear system that arises from the solution of the KSEs in the context of spinorial geometry can be expressed in terms of tensors on the spacetime and their covariant derivatives. In particular, we have that the Nijenhuis tensor is given by and the Lee forms of the Hermitian form ω and of the (4,0) fundamental SU(4) form χ = 4ǫ are given by respectively. The covariant derivative of the Hermitian form is

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where ω αβ = −ig αβ . Furthermore, we have where a ∈ {0, 5}. All these formulae can be used to express the solutions of the linear system in terms of the spinor bilinears. These formulae have also been used to describe the geometry of the supersymmetric backgrounds.

B Spacetime forms from spinor bilinears
To compute the form spinor bilinears of ǫ in (1.1), first note that we can define another spinorǫ = Γ 11 ǫ, which need not be Killing, but is nevertheless defined on the spacetime. Using the Dirac inner product and after an appropriate normalisation of ǫ, we find a 0-form and two 5-forms where ω = −i α e α ∧ eᾱ is the Hermitian form and χ = 4e 1 ∧ e 2 ∧ e 3 ∧ e 4 is the (4,0)-form both of which are the fundamental forms of SU(4).

JHEP12(2015)113 C The linear system for generic SU(4) backgrounds
Here we present a refined form of the linear system associated with the KSEs for generic SU(4) backgrounds, i.e. g 1 = 0. This arises after substituting (1.1) into the KSEs and after some further re-arrangements of the resulting equations. The expressions presented are nearly in the form of a solution to the linear system. The formulae are organised according to representations of SU (4). Moreover, we impose the gauge f 2 = gḡ throughout.
Scalar representation. The conditions that arise in the scalar representation of SU (4) are In addition the following equations restrict components of the H field strength There are also some additional conditions which restrict the remaining fluxes

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It is convenient for the investigation of geometry to rewrite the first set of condition in the 05 frame. One then finds Note also that the conditions on the H flux can be written as This concludes the description of the conditions in the scalar representation.
Hγ 1γ2γ3 + Ωγ 1 ,γ 2γ3 . (C.37) As in the scalar case, it is convenient to re-express the first four equations in the 05 frame to find H 05α = Ω 0,0α − Ω 5,5α , (C.38) where the P ± projectors are defined as follows on any (0,2) tensor G. In the 05 frame the geometric condition above can be rewritten as One can easily see that this follows from L K ǫ = 0.
Traceless (1, 2) representation. Every (1,2) tensor can be decomposed into a traceless component and a trace one as G αβγ =G αβγ + 2 3 g α[β Gγ ]δ δ , whereG denotes the traceless component. Using this, the conditions that transform under the traceless (1, 2) representation are This concludes the description of all conditions on the fields and geometry that arise from the Killing spinor equations.

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D Solution of the linear system for special SU(4) backgrounds The Killing spinor (1.1) for special SU(4) backgrounds is simplified further as g 1 = 0 and thus g = ig 2 . Imposing f 2 = gḡ, one concludes that f = ±g 2 . To derive the conditions on the fields and geometry, we have chosen f = g 2 .
Scalar representation. Imposing f = g 2 on the scalar conditions of the previous section, one finds that Also there is some simplification of the conditions on the G and F fluxes which can be expressed as It may appear that there is an additional geometric constraint in this special case. However, this is not the case. The number of geometric constraints is the same as for the generic backgrounds.

(D.27)
Note that a simplification arises because the derivative of g/ḡ vanishes.
(0, 2) representation. These conditions can now be rewritten as where P ± is defined in (C.49).

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It is the simplification of these equations which allows for a rather simple solution of the linear system. In particular, two equations are automatically satisfied because g 1 = 0 and the remaining conditions are simplified.
Symmetric product of fundamental representations. It is straightforward to see that the conditions now become (1, 2) traceless representation. Finally, the conditions of this representation simplify asH As we shall see all the above conditions can now be solved to express the fluxes in terms of the geometry.

(D.67)
Again the component of the F flux and S that appear in the right-hand side of the above equations are not restricted by the KSEs.
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