Unimodular vs Nilpotent Superfield Approach to Pure dS Supergravity

Recent progress in understanding de Sitter spacetime in supergravity and string theory has led to the development of a four dimensional supergravity with spontaneously broken supersymmetry allowing for de Sitter vacua, also called de Sitter supergravity. One approach makes use of constrained (nilpotent) superfields, while an alternative one couples supergravity to a locally supersymmetric generalization of the Volkov-Akulov goldstino action. These two approaches have been shown to give rise to the same 4D action. A novel approach to de Sitter vacua in supergravity involves the generalisation of unimodular gravity to supergravity using a super-St\"uckelberg mechanism. In this paper, we make a connection between this new approach and the previous two which are in the context of nilpotent superfields and the goldstino brane. We show that upon appropriate field redefinitions, the 4D actions match up to the cubic order in the fields. This points at the possible existence of a more general framework to obtain de Sitter spacetimes from high-energy theories.


Introduction
In recent years there has been significant work on the role of the Volkov-Akulov (VA) goldstino in the spontaneous breaking of local supersymmetry and the generation of a positive contribution to the cosmological constant in supergravity [3][4][5][6][7][8]. In [4] the construction of dS supergravity is based on a constrained (nilpotent) superfield description of the VA action as described for example in [9][10][11][12][13]. In the nilpotent superfield description, the scalar partners of the goldstino are not elementary but composed from goldstino bilinears. An alternative approach to constructing four-dimensional supergravity with spontaneously broken supersymmetry allowing for de Sitter vacua was considered in [2]. The authors considered a locally supersymmetric generalisation of the VA goldstino action describing the dynamics of a space-filling non-BPS 3-brane in 4D N = 1 superspace coupled to the superspace action of minimal N = 1 4D supergravity. They then show that to quadratic order in the goldstino field the action they get coincides with the supergravity constructions using nilpotent superfields.
In [1] three of us took another, very different, approach to dS solutions in supergravity. Specifically, we considered a non-trivial generalisation of unimodular gravity to minimal N = 1 4D supergravity 1 , which allowed for de Sitter solutions. In particular, we formulated a superspace version of the Stückelberg mechanism, which then restored diffeomorphism and local supersymmetry invariance. The cosmological constant and gravitino mass then arise naturally as the vacuum expectation values (vevs) of the components of a Lagrange multiplier superfield after imposing the super-unimodularity condition. At first sight our work [1] is qualitatively different from the constructions using the goldstino brane or equivalently the nilpotent superfield constructions [2,4]. However, it is natural to ask if there is a relationship between our approach and that of [2,4]. This is a step towards understanding whether there is a unique action describing dS in pure supergravity. In this paper we set about answering this question. Although these constructions are all non-perturbative, a direct comparison at that level is very difficult. Therefore, we will do this perturbatively up to the third order in the relevant fields.
In the next section, we briefly highlight the main results of the construction in [2], which we use to connect the results from unimodular supergravity constructions to pure dS supergravity constructions. We then present a brief review of our unimodular supergravity construction [1] in section 3. In section 4 we perturb the unimodular supergravity action up to the cubic order. In section 5 we describe the goldstino dynamics up to the cubic order in unimodular supergravity, which is compared with the goldstino brane action in [2]. We summarise and discuss our results in section 6. Our conventions are summarised in the appendices.

The Goldstino Brane Action in Supergravity
In this section we briefly highlight the main results of the construction of dS supergravity in [2]. The approach there was to couple a local generalisation of the VA action to minimal N = 1 supergravity formulated in superspace [18][19][20]. The starting action in superspace was given by 2 where κ 2 = 8πG N and G N is the gravitational constant, z M = (x µ , θ α ,θβ) are the coordinates of superspace whose curved geometry is described by the supervielbein E A = dz M E A M (z), which contains the fields of the minimal supergravity multiplet [19] and Ber E is the Berezinian of E A M . The superscript (B) denotes the fields used in [2]. This is done to differentiate them from the fields used in our work [1], and the dictionary between the two is given in Appendix A. In (2.1), the first term is the action of standard old minimal supergravity, while the second term gives the anti-de-Sitter cosmological constant term and E is the volume measure of the chiral subspace, ζ M L = (x µ L , Θ α ). The third term in (2.1) is the generalisation of the VA goldstino action, giving the full non-linear contribution of the 3-brane. Its coupling to supergravity is given via its embedding in the bulk superspace as where ξ i are the 3-brane worldvolume coordinates with i = 0, 1, 2, 3. Finally, detE(z(ξ)) denotes the determinant of the pullback of the vector supervielbein, E a (z) = dz M E a M , that is, E a i (z(ξ)) ≡ ∂ i E a (z(ξ)), while the parameter f 2 denotes the 3-brane tension, giving a positive contribution to the cosmological constant. Action (2.1) can be rewritten in chiral subspace using the identity d 6 ζ L E = 2 d 8 z BerE R , where R is the superspace curvature superfield (see appendix B for its components), as follows: where the explicit expression for E is shown later in eqs. (3.8). The component form of action (2.1) can be derived by integrating the first two terms over the Grassmann odd coordinates and fixing the static-gauge x µ (ξ) = δ µ i ξ i on the 3-brane. This gives the action [2] The coupling of the VA goldstino to the supergravity fields is encoded in S V A , where θ α (x) is the VA goldstino. S SG gives standard AdS supergravity, where e = det e a µ , e a µ (x) is the spacetime vielbein, ψ Substituting this into (2.4) and varying with respect to the auxiliary fields b (B) a and M (B) , one can find the solutions to their field equations. Substituting these solutions back into action (2.4) one finally gets, up to the second order in the fermions [2]: In order to compare our results in [1] with those of [2,4], we perturb this action up to the 3rd order in all the field fluctuations, which gives: where D µ is the covariant derivative on the background and we use {...} (3) to denote a perturbation up to the cubic order. We use this notation throughout the paper for the perturbation of the standard part of supergravity. Using the dictionary between the notations in [1] and [2] given in Appendix A, we get the following action: where we have used √ −g = e. This is the action with which we will compare our final result in section 5, where the relations of the fields and parameters in (2.9) and (2.10) will become clear. For example, Λ 2 , the vev of the F-term of the Lagrange multiplier in [1], will be identified with κ 2 f 2 from [2] andG is the goldstino.

Unimodular Gravity and the Stückelberg Procedure
The Stückelberg procedure [22] is a method for reinstating a broken symmetry into the action at the cost of introducing new fields on which the symmetry is realised nonlinearly. We will first illustrate it here in the setting of unimodular gravity which constitutes the starting point for our construction in [1]. Unimodular gravity [23][24][25][26][27][28][29][30] is a restricted version of Einstein-Hilbert gravity, in which the determinant of the metric is fixed to a constant. The most significant difference between unimodular gravity and GR is the way the cosmological constant enters the theory: as an integration constant rather than appearing directly in the action. The action for unimodular gravity in the absence of matter can be written as with 0 being a constant (traditionally set to unity, hence the name "unimodular"). Here Λ(x) is a Lagrange multipler field, imposing a local constraint on the determinant of the metric. This version of the Lagrangian is not invariant under the full diffeomorphism group (Diff) but only under a subgroup of transformations called transverse diffeomorphisms (TDiff), whose parameter 3 ξ T µ satisfies ∇ µ ξ T µ = 0. Since the Lagrange multiplier, Λ(x), transforms like a scalar, it is obvious that Diffs are broken by the last term d 4 xΛ 0 .
We now perform the Stückelberg trick by transforming the Lagrange multiplier under the full group of diffeomorphisms. The transformation rule, written perturbatively in the transformation parameter ξ µ , is: As explained above, the action will not be invariant under this, i.e. S[Λ ] will be a function of ξ µ . We now promote the transformation parameter to a field: ξ µ → φ µ . The Lagrangian can then be constructed order by order in the Stückelberg field φ µ : 3) and it will be invariant, up to the relevant order, when φ µ transforms as 4 : We note that the Stückelberg trick above was performed via an active transformation -i.e. we are transforming the fields and keeping the coordinates fixed. One could alternatively do it via a passive transformation. Non-pertubatively, this involves sending the coordinates and the Stückelberged action will be Of course, upon writing s µ = x µ + φ µ we find that actions (3.6) and (3.3) are identical order by order in φ µ .

Unimodular Supergravity and the Super-Stückelberg Procedure
We are working in the conventions of [19] (see also Appendix B). We find it convenient to work in chiral superspace, where the action of pure N = 1 supergravity is given by The components of R are given in Appendix B and eσ µψ µ , where e = det e a µ , with e a µ the vielbein, ψ µ the gravitino and M the scalar auxiliary field in the old minimal supergravity model. We note that E is the natural supersymmetrisation of the measure √ −g. It is a chiral density superfield, characterised by the transformation law and where is the parameter of local SUSY transformations. For conciseness, we introduced the following notation where ω αβ µ is the spin connection and b µ is the vector auxiliary field in the old minimal model. We define the unimodular supergravity action to be: is now a Lagrange multiplier chiral superfield, and we defined where 0 and m are real constants and the spinor component of E 0 was set to zero for simplicity. Varying over Λ, we get Action (3.12) is invariant under a restricted set of SUSY and diffeomorphism transformations such that they preserve condition (3.15). We remark here that the constraints imposed in eq. (3.15) amount to more than a gauge fixing; in this sense, unimodular supergravity is more than a naive supersymmetrisation of the unimodular gravity model in eq. (3.1). As a consequence, even though the space of solutions of unimodular gravity matches that of standard Einstein gravity with a cosmological constant, it will not be the case for our model. As we will see in subsection 3.3, we are no longer restricted to AdS and flat space backgrounds as one is in standard pure supergravity. Finally, we impose the following boundary conditions on the components of our Lagrange multiplier superfield: where K 0 and K 2 are some constants. We will see in subsection 3.3 how K 0 and K 2 become intimately linked with the cosmological constant in our model. We are now ready to perform the Stückelberg trick in a manner analogous to subsection 3.1. In components, the symmetry breaking terms following from action (3.12) are: We want to perform the Super-Stückelberg trick up to the 2 nd order in the SUSY and diffeomorphism transformation parameters, so we need to know the 2 nd order transformation of the chiral superfield in curved space. This was derived in [1] (working up to the 2 nd order in the fermions): Then, sending ξ µ → φ µ and → ζ we obtain the following action 5 , which is given up to the second order in the Stückelberg fields by: where the "..." stand for terms at higher orders in the Stückelberg fields ζ and φ µ . The action is now invariant under diffeomorphisms and SUSY transformations, provided the Stückelberg fields transform analogously to superspace coordinates (see [1] for details). We remark that the Stückelberg trick can alternatively be applied via passive transformations, in which case the action can be written in the form where Ber ∂Φ ∂X is the Berezinian for the transformation of the superspace coordinates X A as [1] for details). Of course, upon expanding action (3.20), it will coincide with action (3.19) order-by-order in the Stückelberg fields.
Finally, we note that, upon application of the Stückelberg procedure, the boundary conditions (3.16) are modified (to linear order in the Stückelberg fields) as: and are now invariant under diffeomorphisms and SUSY transformations.

Cosmological Constant and Boundary Conditions
We are now interested in the backgrounds allowed by our model, in particular the range of values taken by the cosmological constant. Upon computing the equations of motion following from action (3.19), we find that they admit the solution with all other fields vanishing. The cosmological constant is Thus, our model allows for a cosmological constant of either sign, similar to the results in the constrained superfield literature [2-6, 8, 21, 31-33]. However, we emphasise that in our approach the cosmological constant appears as the combination of the vevs of the Lagrange multiplier superfield components Λ 0 and Λ 2 , which are nothing but the boundary conditions imposed in eqs. (3.21) (note that for our solution the Stückelberg fields vanish on the background).

Unimodular Supergravity at Cubic Order
In this section, we connect the goldstino brane/nilpotent superfield approach to dS vacua, and unimodular supergravity. To this end we perturb the unimodular supersymmetric action shown in eq. (4.1) The fluctuations of √ −g and and of the Pauli matrices, derived from the above fluctuations, can be found at the end of Appendix B.

Terms Cubic in Stückelberg Fields
We now use (4.1) to perturb the unimodular supergravity action (3.19) up to the cubic order in fluctuations. That action will contain terms of the kind L (t 3 ) and L (tχ 2 ) , which are cubic in the Stückelberg fluctuations. These terms could be computed by extending the non-perturbative action (3.19) up to the cubic order in the Stückelberg fields and then perturbing it. This turns out to be quite cumbersome.
However, as we will see below, this proves unnecessary as it is possible to prove that the cubic fluctuations of these terms vanish perturbatively. L (t 3 ) denotes terms cubic in the fluctuation t µ , and L (tχ 2 ) denotes terms linear in t µ and quadratic in the fermionic Stückelberg field χ, together with their hermitian conjugates. L (t 3 ) is the cubic fluctuation of the subset of the Stückelberg action coming from the diffeomorphism transformation. This can easily be computed explicitly and shown to reduce to a total derivative in the perturbatve expansion (remembering that the vevs of Λ 0 and Λ 2 are constant). Taking t µ to vanish on the boundary, we have Now let us look at L (tχ 2 ) . It is of the form where the most general expressions for L A (t µ , χ, χ) 6 and L B (t µ , χ,χ) are given by: It can be checked by explicit computation that and therefore, δL (tχ 2 ) = 0 . One can check that δL A (t µ , χ, χ) + δL B (t µ , χ,χ) = 0 and also δL A (t µ , χ, χ) = 0 = δL B (t µ , χ,χ). So δL (tχ 2 ) can be 0 only if L A (t µ , χ, χ) = L B (t µ , χ,χ) = 0. Hence we see that terms cubic in Stückelberg fields are not present in the cubic action.

Perturbing the Action up to the Cubic Order
In [1] we identified the goldstino, denoted by G, at quadratic order with the combination 9) and the orthogonal mode to G, denoted by τ , as Using these identifications and perturbing action (3.19) by the fluctuations (4.1) up to the 3 rd order, we obtain the action Furthermore, action (4.11) is also invariant under the following supersymmetry transformations (perturbed up to the 2 nd order in fluctuations):

Boundary Conditions and Field Redefinitions
We next look at the perturbations of the boundary conditions, (3.21). Using K 0 = 2 3 m and K 2 = Λ 2 from the background solution (3.22), and the fluctuations (4.1), up to the 2 nd order, we obtain: (4.14) These suggest the following field redefinitions: so that the boundary conditions can now be expressed more simply as We need to substitute the old fields λ 0 , τ and λ 2 by the new fields r 0 , ρ 1 and r 2 . So we invert relations (4.15) up to the 2 nd order, and get, Plugging these expressions for the fields λ 0 , τ and λ 2 into the cubic action (4.11), we get the following action

Goldstino Dynamics
In order to zoom in on the goldstino dynamics in action (4.18), we integrate out the auxiliary fields b µ , M , M * and the Lagrange multipliers r 0 , r * 0 , ρ 1 ,ρ 1 , r 2 and r * 2 . To simplify the process of integrating out the fields, we first perform suitable field redefinitions.
We start by redefining the field b µ as follows: such that the equation of motion of B µ is Nex, we redefine M as follows: Next redefine r 2 as: Because of the boundary conditions (4.16), R 2 vanishes at the boundary: Then the equation of motion of r 0 becomes Now we redefine r 0 as 9) and the equation of motion for R 0 is with the boundary conditionF Next, we find that the following field redefinitions serve to completely decouple t µ from the fermions: From the boundary conditions (4.16) we get The field t µ is redefined as follows: The e.o.m. for R 2 being the same as that of R * 2 implies that the imaginary part of R 2 drops out of the action (which can also be checked explicitly). Now we look at the e.o.m. of P 1 . It is Then we see that because of the boundary condition (5.13), we get Now we plug the solutions for the auxiliary fields B µ , M and M * , and the solutions for the Lagrange multipliers R 0 , R * 0 , P 1 ,P 1 and Re[R 2 ], into the action (4.18). Upon doing so the diffeomorphism Stückelberg field t µ automatically drops out of the action. We finally arrive at the following action: This is the same as action (2.10) which was obtained from [2]. This shows that up to the cubic order in fluctuations the minimal supergravity actions derived from the unimodular and nilpotent superfield approaches, are the same. Action (5.21) has terms only up to the leading order derivatives of the goldstino. We note that other combinations of terms realising supersymmetry nonlinearly can in principle be added to this supergravity action, while keeping it minimal (i.e. without coupling to matter fields). However, they are expected to contain higher order derivatives of the goldstino [34], and may introduce ghost degrees of freedom.

Discussion
In this paper, we have initiated a comparison between two very different approaches to de Sitter supergravity. On the one hand, we have the earlier construction using nilpotent superfields [4], and their elegant realisation as a spacetime filling 3-brane coupled to the minimal N = 1 4D supergravity [2]. On the other hand, we have the supersymmetric generalisation of unimodular gravity proposed in [1]. This includes a Lagrange multiplier chiral superfield that imposes a constraint on the chiral superspace. Supersymmetry is spontaneously broken when the F-term in the Lagrange multiplier picks up a vev, allowing us to source a positive cosmological constant. At first glance, the two formulations are very different. For example, in the former the goldstino of the low energy effective theory is added explicitly. In the latter, it emerges implicitly through the excitations of a Stuckelberg field when the symmetry is spontaneously broken. But then as we showed in section 5, at least up to the cubic order in fluctuations the two actions are related via field redefinitions.
To better understand the similarities and differences between the two models in [1] and [2], it is instructive to look at the superfield version of the action for unimodular supergravity [1]: The background solutions computed in (3.22) suggest that we can definê Up to a constant term, the action can now be written as This should be compared with (2.3) upon use of the relations in Appendix A. In each case, the first terms describe pure AdS supergravity, whereas the second gives the positive contributions to the cosmological constant. The supersymmetry breaking terms look very different, although we have now seen how they are equivalent up to cubic order in perturbations about the de Sitter vacuum solution, as shown in section 4 and section 5. Given the manifestly distinct starting points for the different constructions, this is an intriguing result. Moreover, in general, a locally supersymmetric action giving rise to dS solutions is not expected to be unique. An example of a term not present in our construction is: √ẽg µνψ µψν , (6.6) where we used the invariant vielbein and gravitino combinations e a µ = e a µ +D µ X a + 2iθσ aψ µ − 2iψ µ σ aθ + iθσ aD µθ − iD µ θσ aθ , ψ µ = ψ µ +D µ θ . (6.7) These are constructed by Volkov-Soroka as in [35][36][37], whereD denotes a covariant derivative w.r.t. an independent connectionω µ (x) introduced in [35][36][37]. Note that X a is the Stückelberg field for local Poincaré translations. However, term (6.6) is expected to contain a ghost degree of freedom (as can be seen by looking at the linearised approximation in [38]). The fact that both models failed to produce any of these (potentially pathological) terms might suggest a common origin in terms of a consistent underlying theory. The equivalence between the two theories remains to be shown to higher order. If equivalence can be shown, there would be compelling evidence for a more comprehensive (and perhaps more natural) construction, either at higher energies or higher N . These superficially distinct formulations would be understood as following from different procedures for going to lower energies or (spontaneously) breaking the SUSY, but ultimately leading to the same physics. This putative theory would then have the potential to give an explanation at a more fundamental level for the different constraints employed in the models we looked at in this paper. On the other hand, if higher order effects reveal a fundamental difference in the two set-ups, it would be interesting to explore the phenomenological consequences in greater detail. We note with interest the recent application of nilpotent superfields as a natural way to project out certain Standard Model contributions to the vacuum energy [39]. Could these methods also be adapted to a super-unimodular framework?

Superfield R
The chiral supergravity superfield R in component form is: