Three-form multiplet and supersymmetry breaking

Recently, a nilpotent real scalar superfield V was introduced in [1] as a model for the Goldstino. It contains only two independent component fields, the Goldstino and the auxiliary D-field. Here we first show that V can equivalently be realised as a constrained three-form superfield. We demonstrate that every irreducible Goldstino superfield (of which the Goldstino is the only independent component field) can be realised as a descendant of V which is invariant under local rescalings V → eτV, where τ is an arbitrary real scalar superfield. We next propose a new Goldstino supermultiplet which is described by a nilpotent three-form superfield Y\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{Y} $$\end{document} that is a variant formulation for the nilpotent chiral superfield, which is often used in off-shell models for spontaneously broken supergravity. It is shown that the action describing the dynamics of Y\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{Y} $$\end{document} may be obtained from a super-symmetric nonlinear σ-model in the infrared limit. Unlike V , the Goldstino superfield Y\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{Y} $$\end{document} contains two independent auxiliary fields, F = H + iG, of which H is a scalar and G is the field strength of a gauge three-form. When Y\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{Y} $$\end{document} is coupled to supergravity, both H and G produce positive contributions to the cosmological constant. While the contribution from H is uniquely determined by the parameter of the supersymmetry breaking in the action, the contribution from G is dynamical.


Introduction
Recently, a new Goldstino superfield for spontaneously broken N = 1 supersymmetry in four spacetime dimensions has been introduced [1]. In the super-Poincaré case, it is described by a real scalar superfield V subject to the nilpotency constraints where D A = (∂ a , D α ,Dα) are the covariant derivatives of N = 1 Minkowski superspace M 4|4 . These nilpotency constraints have to be supplemented with the requirement that the descendant D α W α =DαWα is nowhere vanishing, where The nilpotency constraints (1.1) imply that V has two independent component fields 1 which are: the Goldstino, which may be identified with W α | θ=0 , and the auxiliary D-field being proportional to D α W α | θ=0 . All other component fields of V are composite ones. In particular, from (1.1) one may deduce the representation V → e τ V , (1.5) where τ is an arbitrary real scalar superfield. Requiring the action (1.4) to be stationary under arbitrary variations of the form δV = τ V leads to the following constraint which proves to express the auxiliary field in terms of the Goldstino. The constraints (1.1) and (1.6) define the irreducible Goldstino superfield V described in [2]. An explicit realisation for V was given long ago by Lindström and Roček [3] in the form where φ is the irreducible chiral scalar Goldstino superfield [4,5],Dαφ = 0, which is subject to the constraints [4]: (1.8b) Another useful realisation for V is where Σ is the Goldstino superfield introduced in [6]. It obeys the improved complex linear constraint as well as it is nilpotent and is subject to a holomorphic nonlinear constraint, In this paper we uncover new interesting properties of the Goldstino multiplet V . In particular, we show that V can equivalently be realised as a constrained three-form superfield. We also demonstrate that every irreducible Goldstino superfield 2 can be realised JHEP09(2017)089 as a descendant of V , which is invariant under local rescalings V → e τ V , where τ is an arbitrary real scalar superfield.
In the last two years, there has been much interest in models for off-shell N = 1 supergravity coupled to nilpotent Goldstino superfields. One of the main reasons for such interest is that every Goldstino superfield coupled to supergravity provides a positive contribution to the cosmological constant [2,3,[8][9][10][11], unlike the supersymmetric cosmological term [12] which yields a negative contribution to the cosmological constant. The same property holds for the Goldstino brane [13]. All irreducible Goldstino superfields provide one and the same universal contribution to the cosmological constant [2], in accordance with the super-Higgs effect [14][15][16]. Exactly the same contribution is generated by the known reducible Goldstino multiplets, which are: (i) the superfield V discussed above; and (ii) the nilpotent chiral superfield X [17,18] used in numerous recent publications including [8][9][10]. In this paper we introduce a new reducible Goldstino superfield, a nilpotent three-form multiplet, which will be shown to provide two separate positive contributions to the cosmological constant, of which one is universal and the other is dynamical.
2 From V to equivalent three-form multiplet We start by recalling two simple models for spontaneously broken supersymmetry that are realised in terms of an unconstrained real scalar superfield V . One of them describes an abelian vector multiplet with action which is obtained by adding a Fayet-Iliopoulos term [7] to the massless vector multiplet action. The functional (2.1) is invariant under gauge transformations δV = λ +λ ,Dαλ = 0 . (2. 2) The chiral spinor W α defined by (1.2) is a gauge-invariant field strength for this model. Our second model describes the dynamics of a variant scalar multiplet known as the three-form multiplet [19,20] (see [21] for a review). We choose the action where the chiral scalar superfield Ψ,DαΨ = 0, is defined by It is called the three-form multiplet. Its specific feature is the relation which means that the auxiliary F -field of Ψ, defined by F = − 1 4 D 2 Ψ| θ=0 , is a complex scalar such that its imaginary part, ImF , is the divergence of a vector (or, equivalently, the JHEP09(2017)089 field strength of a gauge three-form). This is the only difference between the three-form multiplet and the standard scalar multipelt.
The field strength (2.4)  where L is an arbitrary linear multiplet. This gauge symmetry corresponds to a gauge theory with linearly dependent generators, following the terminology of the Batalin-Vilkovisky quantisation [22], and therefore the quantisation of (2.3) cannot be carried out using the Faddeev-Popov procedure. 3 The supersymmetric theories (2.1) and (2.3) describe the dynamics of two different multiplets, the vector and the scalar ones, respectively, if the dynamical superfield V is unconstrained. However, in case V is subject to the nilpotency constraints (1.1), which are incompatible with the gauge symmetries (2.2) and (2.6), any difference between the actions (2.1) and (2.3) proves to disappear. Once the constraints (1.1) are taken into account, the action (2.1) (which coincides with the right-hand side of (1.4) modulo a total derivative) can be rewritten in the form (2.3). As a consequence of (1.1), the chiral scalar Ψ proves to be nilpotent, It also obeys the nonlinear constraint which expresses the field strength of the gauge three-form, ImF , in terms of the Goldstino and ReF . The latter constraint follows from the observation that (1.3) may be rewritten in several equivalent forms (2.8) The above analysis demonstrates that the Goldstino multiplet V under the nilpotency conditions (1.1) is equivalent to the chiral superfield Ψ subject to the constraints (2.7). Therefore, the description in terms of Ψ provides a different realisation of the same multiplet.
It is also worth pointing out that the chiral superfield φ defined by (1.8) is the threeform multiplet associated with the irreducible Goldstino superfield V defined by the constraints (1.1) and (1.6), JHEP09(2017)089

Irreducible and reducible Goldstino superfields
In accordance with the discussion in [2], there are two general types of N = 1 Goldstino superfields, irreducible and reducible ones. Every irreducible Goldstino superfield contains only one independent component field -the Goldstino itself, while the other component fields are composites constructed from the Goldstino. 4 Given an irreducible Goldstino superfield, the corresponding component action can be related to the Volkov-Akulov action [25][26][27] using the formalism developed in [28]. Every reducible Goldstino superfield contains at least two independent fields, one of which is the Goldstino and the other fields are auxiliary (the latter become descendants of the Goldstino on the mass shell). Examples of irreducible Goldstino superfields are the chiral scalar (1.8) and the complex linear scalar (1.10). The well-known example of a reducible Goldstino superfield was introduced in [17,18]. It is a chiral scalar X ,DαX = 0, which is subject to the nilpotency constraint in conjunction with the requirement that the descendant D 2 X is nowhere vanishing. The dynamics of this supermultiplet is described by the action As was pointed out in [2], the nilpotency condition (3.1) is preserved if X is locally rescaled, Requiring the action (3.2) to be stationary under such re-scalings of X (see [1]) gives where φ is Roček's chiral scalar defined by (1.8).
As was demonstrated in [6] (see also [2,29]), every irreducible Goldstino superfield can be expressed in terms of the complex linear Goldstino superfield Σ, eq. (1.10), and its conjugateΣ. On the other hand, Σ can be represented as a descendant of the reducible Goldstino superfield V subject to the constraints (1.1). The corresponding realisation is A remarkable feature of this representation is that Σ proves to be invariant under local re-scalings (1.5) of V ,

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Here τ is an arbitrary real scalar superfield. Since every irreducible Goldstino superfield is a descendant of Σ andΣ, we conclude that all irreducible Goldstino superfields are invariant under local re-scalings (1.5) of V . This includes the real Goldstino superfield V given by (1.9), with Σ realised as in (3.5). Now let us note that a transformation (1.5), where V is subject to (1.1) rescales the auxiliary field. Hence, the invariance of Σ under this transformation means that Σ does not contain the auxiliary field and describes an irreducible Goldstino model. This observation also explains why all irreducible Goldstino models (which contain only the Goldstino and no auxiliary fields) are invariant under re-scaling of V .
As was noticed in [2], every reducible Goldstino superfield can always be represented as an irreducible one plus a "matter" superfield, which contains all the auxiliary component fields. In our case, the reducible Goldstino superfield V can be realised as where Σ is given by (3.5). The "matter" superfield U obeys the generalised nilpotency condition and transforms under (3.6) as The superfield U contains only one independent component field, which is the auxiliary field of V . It should be remarked that Σ can also be expressed in terms ofX as

Nilpotent three-form Goldstino multiplet
In this section, we introduce a new reducible Goldstino superfield. It is a three-form multiplet, which is constrained to be nilpotent, with h =h a positive parameter. This nilpotent three-form multiplet is a variant formulation of the nilpotent chiral multiplet X discussed in the previous section.
Interesting enough, the above theory can be obtained from a nonlinear σ-model action in the infrared limit, as an extension of the approach advocated in [17]. Let us define the components of Y as As was already explained in eq. (2.5) it follows from (4.1a) that G is a divergence of a vector which we denote by C a , that is G = ∂ a C a . Equivalently, * G = dC for some three-form potential C. The action (4.3) in components is just the standard action for a supersymmetric nonlinear σ-model The equations of motion for the auxiliary fields H and C a are given by which lead to

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where g is an arbitrary constant. Substituting (4.9) into the action (4.5), (4.7) we obtain the scalar potential V (ϕ,φ) = K −1 ϕφ (W ϕ + ig)(Wφ − ig) . (4.10) Note that it receives contributions from both the bulk and boundary actions. Let us choose Kähler normal coordinates in the σ-model target space near the vacuum so that in the vacuum where R is the curvature of the target space. Then the vacuum is determined by the equation We are interested in a supersymmetry breaking solution for which F ∼ Wφ − ig = 0. This means that W ϕϕ = 0. The vacuum energy is given by Since W ϕϕ = 0, the fermion ψ is massless and becomes a Goldstino. In addition, we have two massive scalar fields. For simplicity let us assume that the supersymmetry breaking vacuum is located at ϕ =φ = 0. Denoting where for simplicity we have assumed that h and w are real, and expanding the action to quadratic order in fluctuations we find that the masses of the scalar fields are where f = h + ig. To make sure that they both are positive we have to require that R < 0. To find the theory of just the Goldstino ψ we decouple the scalar fields by taking their masses to infinity. For this we take the limit of infinite curvature |R| → ∞. The leading contribution to the action (4.5) in this limit is This gives the following equation of motion for φ It is clear that this equation is solved by
Since S div = 0 on the solution (4.18) the action for the remaining fields ψ, H, G comes from the subleading terms in the action (4.5) Note that this is just the component form of the superfield action (4.2). This action should be supplemented by the boundary term (4.20) The auxiliary fields H and G can be eliminated using their equations of motion which gives Eq. (4.21b) is solved by for some constant g. Eqs. (4.21a) and (4.22) can also be written as where, as before, f = h + ig.

Models for spontaneously broken supergravity
In describing supergravity-matter systems in superspace, it is useful, following the ideas pioneered in [32,33], to formulate every pure supergravity theory as conformal supergravity coupled to a compensating supermultiplet. Different off-shell formulations for supergravity correspond to different compensators [21,34]. Conformal supergravity can be realised using the supergravity multiplet described in terms of the superspace geometry of [35,36] (which underlies the Wess-Zumino approach [37] to the old minimal formulation for N = 1 supergravity developed independently in [38,39]) augmented with the super-Weyl invariance of [40]. An infinitesimal super-Weyl transformation has the form where σ is an arbitrary covariantly chiral scalar superfield,Dασ = 0.

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There are several natural ways to lift the Goldstino superfield V , which was described in section 1, to supergravity. Of course, the constraints (1.1) are generalised to curved superspace in the unique way given in [1,2]: Non-uniqueness occurs when choosing a super-Weyl transformation for V . In this paper we consider the following transformation laws: and In both cases, the constraints (5.2) are super-Weyl invariant. One can choose a more general super-Weyl transformation law for V of the form δ σ V = a(σ +σ)V , for some parameter a, by multiplying V (I) by some power of the compensator used. In particular, the choice a = −1 was made in [2] to describe the Goldstino brane.

Super-Weyl inert V
Let us assign the super-Weyl transformation law (5.3) to the Goldstino superfield V . Then the coupling of the old minimal supergravity [37][38][39] to V is described by the super-Weyl invariant action [1] Here S 0 the chiral compensator,DαS 0 = 0, with the super-Weyl transformation δ σ S 0 = σS 0 . 6 The functional in the first line of (5.5) is the old minimal supergravity action, in which the expression in the figure brackets is the supersymmetric cosmological term [42,43]. Within the new minimal formulation for N = 1 supergravity [45] (see also [46,47]), the compensator is a real covariantly linear scalar superfield, with the super-Weyl transformation δ σ L = (σ +σ)L. The action for supergravity coupled to the Goldstino superfield V is [1]

7)
6 Here E is the full superspace measure, and E denotes the chiral density. We use the notation S0 for the chiral compensator following [34,41]. In the superspace literature, the chiral compensator is usually denoted Φ, see e.g. section 6.6.1 in [24].

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where S 0 is a covariantly chiral scalar superfield,DαS 0 = 0 (it is a purely gauge degree of freedom). The first term in (5.7) corresponds to the new minimal supergravity action. An important feature of unbroken new minimal supergravity is that it does not allow any supersymmetric cosmological term [46,47]. 7

Super-Weyl non-invariant V
If the Goldstino superfield V is chosen to possess the super-Weyl transformation law (5.4), then we can associate with it the following three-form superfield It is nilpotent, Ψ 2 = 0, as a consequence of (5.2). It transforms as a primary superfield under the super-Weyl group, The action for old minimal supergravity coupled to the Goldstino superfield Ψ is 10) This model is equivalent to (5.5).

Three-form supergravity
In 1981, Gates and Siegel [20] proposed a variant formulation of the old minimal supergravity, which is obtained from the supergravity action given in [48] by replacing the compensating chiral scalar superfield with a three-form superfield. 8 At the component level, this supergravity formulation was elaborated in [50] where is was called "three-form supergravity." The modern prepotential formulation for three-form supergravity was given in appendix B of [51]. Further aspects of three-form supergravity were studied in [52].
Here we describe three-form supergravity following [51]. This supergravity formulation is obtained from the old minimal theory by replacing S 3 0 with where the prepotential P is a real scalar superfield such that Ξ is nowhere vanishing. The super-Weyl transformation of P is defined to be δ σ P = (σ +σ)P . (5.12) 7 Among the known off-shell formulations for N = 1 supergravity (see [21,24] for reviews), supersymmetric cosmological terms exist only for the old minimal supergravity [42,43] (and its variant version reviewed in section 5.3 below) and the n = −1 non-minimal supergravity of [44]. 8 Probably the first serious study of matter three-form multiplets coupled to supergravity was given in [23]. A superform formulation for the three-form multiplet in a supergravity background was given in [49].

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Then the chiral superfield Ξ transforms as The pure supergravity action is Here the second term on the right is a supersymmetric cosmological term. The supergravity action (5.14) is invariant under gauge transformations which leave invariant the chiral superfield Ξ 3 defined by (5.11). The equation of motion for P is Here the chiral scalar R is invariant under the super-Weyl transformations. The general solution to the equation of motion is R = m + ie, for some real parameter e.

Three-form Goldstino superfield in supergravity
The nilpotent three-form multiplet (4.1) is naturally lifted to supergravity. In curved superspace, its gauge-invariant field strength is defined by This chiral scalar is constrained to be nilpotent, in conjunction with the requirement that the descendant D 2 Y is nowhere vanishing. The prepotential U in (5.17a) is postulated to possess the super-Weyl transformation δ σ U = (σ +σ)U , (5.18) which implies that Y is transforms as a super-Weyl primary superfield, The chiral scalar Y defined by (5.17a) is invariant under gauge transformations of U of the type (5.15). The action for old minimal supergravity coupled to the Goldstino superfield Y is

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In the flat superspace limit it reduces to (4.2). This action should be supplemented by a boundary term generalising (4.20). As discussed in section 4, the Goldstino superfield Y contains two independent auxiliary fields, F = H + iG, of which H is a scalar and G is the field strength of a gauge threeform. In supergravity, both H and G produce positive contributions to the cosmological constant. While the contribution from H is uniquely determined by the parameter of the supersymmetry breaking h in (5.20), the contribution from G is dynamical. We believe that the latter may be used to neutralise the negative contribution from the supersymmetric cosmological term.
The idea that massless gauge three-forms make it possible to generate a cosmological constant dynamically, has attracted much interest since the early 1980s [30,[53][54][55][56][57][58]. We believe it will be useful in the framework of spontaneously broken local supersymmetry.
After this work had been submitted to the hep-th archive, we became aware of the recent paper [59] in which the nilpotent three-form multiplet was also studied and used for different purposes.