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Cosmology with Orthogonal Nilpotent Superfields

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Cosmology with Orthogonal Nilpotent Superfields Cosmology with orthogonal nilpotent superfields The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Ferrara, Sergio, Renata Kallosh, and Jesse Thaler. "Cosmology with orthogonal nilpotent superfields." Phys. Rev. D 93, 043516 (February 2016). As Published http://dx.doi.org/10.1103/PhysRevD.93.043516 Publisher American Physical Society Version Final published version Citable link http://hdl.handle.net/1721.1/101156 Terms of Use Creative Commons Attribution Detailed Terms http://creativecommons.org/licenses/by/3.0 PHYSICAL REVIEW D 93, 043516 (2016) Cosmology with orthogonal nilpotent superfields † ‡ Sergio Ferrara,1,2,3,* Renata Kallosh,4, and Jesse Thaler5, 1Theoretical Physics Department, CERN CH1211 Geneva 23, Switzerland 2INFN–Laboratori Nazionali di Frascati Via Enrico Fermi 40, I-00044 Frascati, Italy 3Department of Physics and Astronomy, University of California, Los Angeles, California 90095-1547, USA 4SITP and Department of Physics, Stanford University, Stanford, California 94305, USA 5Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA (Received 8 December 2015; published 9 February 2016) We study the application of a supersymmetric model with two constrained supermultiplets to inflationary cosmology. The first superfield S is a stabilizer chiral superfield satisfying a nilpotency condition of degree 2, S2 ¼ 0. The second superfield Φ is the inflaton chiral superfield, which can be B ≡ 1 ðΦ − Φ¯ Þ B S SB ¼ 0 combined into a real superfield 2i . The real superfield is orthogonal to , , and satisfies a nilpotency condition of degree 3, B3 ¼ 0. We show that these constraints remove from the spectrum the complex scalar sgoldstino, the real scalar inflaton partner (i.e. the “sinflaton”), and the fermionic inflatino. The corresponding supergravity model with de Sitter vacua describes a graviton, a massive gravitino, and one real scalar inflaton, with both the goldstino and inflatino being absent in unitary gauge. We also discuss relaxed superfield constraints where S2 ¼ 0 and SΦ¯ is chiral, which removes the sgoldstino and inflatino, but leaves the sinflaton in the spectrum. The cosmological model building in both of these inflatino-less models offers some advantages over existing constructions. DOI: 10.1103/PhysRevD.93.043516 I. INTRODUCTION also be realized nonlinearly. In such cases, the corresponding goldstino multiplet contains a spin-1=2 fermion, but it does De Sitter space plays a crucial role in our current under- not contain a spin-0 or spin-1 partner; rather, a nonlinear standing of cosmological observations [1]. The inflationary epoch in the early universe occurs in approximate de Sitter supersymmetry operation flips a one-particle fermion state space, and the present day acceleration of the universe will into a two-particle fermion state. It was recognized a long lead to de Sitter space asymptotically. If supersymmetry is time ago in [4] that nonlinear realizations of supersymmetry realized in nature, then it must be spontaneously broken can also be described using constrained superfields, and during any de Sitter phase. It is therefore interesting to study interest in constrained multiplets was renewed in [5,6]. de Sitter vacua with spontaneously broken local supersym- While constrained multiplets were originally introduced metry, especially in cases where the interaction of matter for global supersymmetry, they can be consistently gener- with gravity is an essential ingredient. alized to local supersymmetry, as will be explained below. In a cosmological context, one can ask whether super- In this paper, we show how single-field inflation can be symmetry is linearly or nonlinearly realized in a de Sitter consistently embedded in local supergravity with the help of phase. Standard linear multiplets involve partner particles constrained multiplets. The resulting supergravity action is which differ by a half-unit of spin [2]: spin-0 scalars with surprisingly economical, since it describes the dynamics of spin-1=2 fermions, spin-1=2 fermions with spin-1 vectors, just a single real inflaton, a graviton, and a massive gravitino. spin-3=2 gravitino with spin-2 graviton, and so on. These Our construction uses the superfield content of [7],withtwo supermultiplets form representations of the superalgebra constrained chiral multiplets S and Φ. The stabilizer field S 1 and the supersymmetry operation flips the spin of the state satisfies a nilpotency condition of degree 2, by 1=2. It was first recognized in [3] by Volkov-Akulov S2 ¼ 0 ð Þ (VA) that spontaneously broken global supersymmetry can ; 1:1 and the inflaton is embedded in an orthogonal multiplet Φ *[email protected] † satisfying [email protected] ‡ [email protected] 1We use the terms “nilpotent” and degree of nilpotency as if Published by the American Physical Society under the terms of superfields were square matrices: a superfield Xðx; θ; θ¯Þ is the Creative Commons Attribution 3.0 License. Further distri- nilpotent of degree r if r is the least positive integer such that bution of this work must maintain attribution to the author(s) and Xr ¼ 0. The term “orthogonal” will be used here as in the case of the published article’s title, journal citation, and DOI. vectors: two superfields X and Y are orthogonal if XY ¼ 0. 2470-0010=2016=93(4)=043516(15) 043516-1 Published by the American Physical Society FERRARA, KALLOSH, and THALER PHYSICAL REVIEW D 93, 043516 (2016) 1 constant in local supersymmetry, the S multiplet always SB ¼ 0; B ≡ ðΦ − Φ¯ Þ: ð1:2Þ 2i contributes a positive cosmological constant, so it naturally appears in studies of de Sitter space. The minimal case of The real superfield B also satisfies a nilpotency condition of local supersymmetry coupled just to S leads to a nonlinear degree 3, B3 ¼ 0 [5]. Naively, a chiral inflaton muliplet Φ realization of pure de Sitter supergravity without low would contain a fermionic inflatino partner and an additional “ ” 2 energy scalars [23,24]. The action is complete with all real sinflaton scalar partner, but such states are absent in higher order fermion couplings, and this complete locally the nonlinear realization. As we will explain, this presents supersymmetric action can be subsequently coupled to new opportunities for inflationary model building, since matter fields [24–26]. In string theory, nilpotent multiplets cosmological challenges presented by the inflatino and arise [27,28] when constructing supersymmetric versions sinflaton are now absent. of Kachru-Kallosh-Linde-Trivedi (KKLT) uplifting to de S2 ¼ 0 The importance of the constraint for cosmology Sitter vacua [29].4 The nilpotent multiplet plays an impor- S is already well known. The unconstrained linear multiplet tant role in KKLT and large volume scenario moduli has components stabilization scenarios, in particular for applications to particle phenomenology and cosmology [33]. Nilpotent S ¼ðS; χs;FsÞ; ð1:3Þ multiplets also appear in studies of supersymmetry break- where χs is the goldstino, S is its scalar partner (i.e. the ing with multiple “goldstini” [34]. In our view, the fact that sgoldstino), and the Fs auxiliary field is the order parameter the complete VA nonlinear goldstino action appears on the for supersymmetry breaking. While there have been D-brane world-volume in string theory [27] suggests that attempts to identify the sgoldstino with the inflaton [8], the consideration of constrained versus unconstrained sgoldstino inflation scenarios face a number of challenges multiplets (and linear versus nonlinear realizations) is [9]. Therefore, it is typically necessary to stabilize S and broader issue than originally envisaged. decouple it from cosmological evolution. For example, in The goal of this paper is apply the logic of nonlinear realizations and superfield constraints to the inflaton itself. the case of a supergravity version of the Starobinsky model, Φ one can use a linear realization of supersymmetry [10] and The unconstrained inflaton multiplet has components ¯ 2 stabilize the sgoldstino via a Kähler potential term −cðSSÞ Φ ¼ðφ þ ib; χϕ;FϕÞ; ð1:4Þ [11]. More economically and elegantly, though, one can use where φ is the inflaton, b is the sinflaton, χϕ is the inflatino, a nonlinear realization of supersymmetry and simply ϕ remove the sgoldstino via the S2 ¼ 0 constraint [12] and and F is an auxiliary field. Just as the nilpotency S2 ¼ 0 in this way one can build the bosonic part of Volkov- constraint projects out the sgoldstino S and replaces Akulov-Starobinsky supergravity.3 it with a goldstino bilinear term, the orthogonality con- SB ¼ 0 χϕ ϕ A proposal to use the nilpotent multiplet in a general straint implies that b, , and F are no longer independent fields and are instead functionals of χs, Fs, and class of cosmological models was made in [13], starting φ with Lagrange multipliers in the superconformal models . The fact that superfield constraints reduce the total underlying supergravity. The stabilizer field S with S2 ¼ 0 number of physical low energy degrees of freedom was one of the motivations for the study of such constrained is now known as a nilpotent multiplet, and the resulting systems. The relevance of the constrained S and Φ fields inflationary models are known as “sgoldstino-less” models. for cosmological applications was described in [7] in the By now, there are various cosmological inflationary models context of building a minimal supersymmetric EFT for consistent with the data and yielding supersymmetry – fluctuations about a fixed inflationary background. Here, breaking at the minimum of the potential [14 17]. Many we are interested in studying the full inflationary dynamics, recent developments on sgoldstino-less models were including the end of inflation. described in [18,19], as well as other directions of work For cosmological applications, the key feature of these with constrained superfields. There are also supersymmet- orthogonal nilpotent superfields is that they have a particu- ric effective field theories (EFTs) of inflation [20,21] built larly simple form when χs ¼ 0.
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