Reheating after inflation by supersymmetry breaking

We study reheating after the end of inflation in models where the inflaton is the superpartner of goldstino and is charged under a gauged $U(1)$ R-symmetry. We consider two classes of models -- one is small field characterized by an almost flat K\"ahler space, and the other large field characterized by a hyperbolic K\"ahler space $SU(1,1)/U(1)$, while in both cases the inflaton superpotential is linear due to the R-symmetry. The inflationary observables of our models fit within 2$\sigma$ CMB values. Upon coupling the inflaton sector to the (supersymmetric) Standard Model, we compute the MSSM parameters, mass spectrum, and decay modes of the inflaton, with the resulting reheating temperature around $10^8$ GeV. We also find that both models can accommodate superheavy LSP dark matter, depending on the parameter choice.


Introduction
In past works, a framework of natural inflation within supergravity was proposed, dubbed 'inflation by supersymmetry breaking' [1,2]. The main idea is to identify the inflaton with the superpartner of the goldstino, in the presence of a gauged R-symmetry. The minimal field content consists of the inflaton chiral superfield Z charged under an abelian Maxwell multiplet gauging the R-symmetry. The superpotential is then fixed by symmetry to be linear in Z, spontaneously breaking supersymmetry and in general R-symmetry with the gauge boson becoming massive by absorbing the phase of the inflaton. On the other hand, the Kähler potential can be expanded around the origin Z = 0 which corresponds to a maximum of the scalar potential, where R-symmetry is restored. In the limit of vanishing gauge coupling, at the lowest order (canonical Kähler potential) the slow-roll parameter η vanishes, while its first correction determines η. One therefore obtains a natural small-field hilltop type inflation around the maximum, ending as the inflaton rolls down towards the minimum. The latter is controlled by the second order correction and the D-term contribution which can tune the vacuum energy to zero, or a tiny positive value corresponding to the dark energy of the observable universe.
In this work, we couple the inflaton and supersymmetry breaking sector described above with the (supersymmetric) Standard Model (MSSM) and study the reheating after the end of inflation. In particular, we compute the superparticle spectrum [3], the decay modes of the inflaton and the resulting reheating temperature. In principle, there are two distinct possibilities for the MSSM superpotential Ω: (1) to be neutral under the R-symmetry, in which case the full superpotential is proportional to the goldstino superfield Z and Ω is added to the goldstino decay constant; (2) to have the same R-charge as Z so that Standard Model particles are neutral while their superpartners are charged, in which case Ω is just added to the supersymmetry breaking sector superpotential. Note that in this case the gauged R-symmetry contains the usual R-symmetry of the MSSM [4]. It turns out that both possibilities lead to similar results and thus we choose to perform the explicit analysis for case (1) and then (in the concluding section) comment on the corresponding changes for case (2). Of course, one could have more general situations with different R-charges that can be studied by extending our analysis in a straightforward way.
The outline of our paper is the following. In Section 2, we review briefly the framework of inflation by supersymmetry breaking and describe the coupling of the supersymmetry breaking sector to the MSSM. In Section 3, we specialise to a Kähler potential perturbatively expanded around the canonically flat case, compute the superparticle spectrum (soft scalar masses, gaugino masses and trilinear couplings), and calculate the decay modes of the inflaton and the resulting reheating temperature. In Section 4, we repeat the analysis for a non-flat hyperbolic Kähler potential. In Section 5, we consider the effects introducing Z-dependent wavefunctions for the matter fields in the Kähler potential, and derive the requirements for vacuum stability. In Section 6, we discuss Dark Matter possibilities within our model. Finally in Section 7, we present our conclusions, while in the Appendix we give the supergravity Lagrangian that we use throughout the paper.

General setup
The starting point is a class of models with gauged U (1) R phase symmetry, defined by Kähler potential and superpotential (κ = M −1 P is the gravitational constant), where Z is the inflaton/sgoldstino superfield, φ collectively denotes matter superfields, and J is the inflaton Kähler potential. In the superpotential, a is a dimensionless real constant, while Ω is the MSSM part, Hereū,d,ē, Q, L, H u , H d are chiral superfields. As usual, we denote the corresponding SM matter fields (quarks, leptons, and Higgs fields) with the same character, while tildes will be used for their superpartners (squarks, sleptons, and Higgsinos). The un-normalized Yukawa couplings y and the µ-parameter are denoted by hats which will be removed after proper rescaling, once Z settles at the minimum. The total gauge group of the model is, Squarks, sleptons, and Higgs scalars are neutral under U (1) R , while Z carries the same R-charge as the superpotential. The R-charges of the MSSM fermions will be fixed later. The scalar potential is the sum Here the indices I, J run through all the chiral (super)fields, while A, B are the gauge group indices. The relevant part of supergravity Lagrangian that we use here can be found in the Appendix and its derivation in Ref. [5].
For the gauge kinetic matrix the following notation is used, f AB ≡ f −1 AB . Kähler covariant derivatives are defined as D I W ≡ W I + κ 2 K I W , where the indices denote the respective partial derivatives. The Killing potential and Killing vector are related by where the gauge couplings and charges are included in the Killing vectors X I A . For example, if Z transforms under U (1) R as Z → Ze −igqϑ (where ϑ is a transformation parameter and q is its R-charge), its Killing vector is X Z R = −igqZ. The gauge couplings of U (1) R , U (1) Y , SU (2) L , and SU (3) c are g, g 1 , g 2 , and g 3 , respectively.
We use a convention where the superpotential transforms under U (1) R with unit Rcharge, W → W e −igϑ , and the fermionic superspace coordinate transforms with half-unit R-charge, θ → θe −igϑ/2 . Then Z has unit R-charge, while its fermionic partner has half-unit R-charge. In general, for a scalar field with R-charge q, its fermionic partner has R-charge q − 1/2. With this convention let us write down in Table 1 the fermion charges under the total gauge group of our model.
In this class of models, the Z-dependent part of the potential drives inflation, after which Z and its auxiliary field F Z settle at non-zero vacuum expectation values (VEVs), spontaneously breaking both supersymmetry (SUSY) and U (1) R . At the vacuum, the gravitino Table 1: MSSM and U (1) R charges of the fermions. ζ is the inflatino, λ R is the U (1) R gaugino, and λ 1,2,3 are bino, wino, and gluino, respectively. The gravitino has the same R-charge as λ R . mass and the the auxiliary fields of Z and U (1) R are given by, where we assume that matter fields φ vanish at the minimum.
The Yukawa couplingsŷ and the parameterμ in (3) are related to their properly normalized versions as This is due to the overall factor of e K in the F -term potential, as well as the coupling of Ω to Z as shown in Eq. (2). At the vacuum, Z and J(Z, Z) take non-vanishing VEVs, which leads to this rescaling. As for the inflaton part J of the Kähler potential, we consider two examples described below.

Model I: (almost) flat Kähler space
Since we require that matter fields vanish at the minimum, vacuum structure is defined entirely by the choice of the Kähler potential J(Z, Z) (as the superpotential is already fixed). One example of a suitable (for inflation and SUSY breaking) almost canonical Kähler potential was given in Ref. [1], which uses a non-perturbative correction of the form ∼ ZZe κ 2 ZZ . Here we would like to introduce a simpler choice of J with finite number of perturbative corrections, namely, where the parameters α and β are dimensionless. One should think of the above form as a perturbative expansion around the canonical kinetic terms with coefficients less than unity.
However in this case the potential is convex (V ZZ > 0) around Z = 0 and slow-roll hilltop inflation is not possible. The problem is solved if we add small α. One example of a suitable scalar potential is given by the parameter choice with the inflaton VEV | κZ | = 1.22. 2 This gives rise to inflation with n s = 0.9615 , r = 8.85 × 10 −5 , H inf = 2.33 × 10 12 GeV , for 60 e-folds. The scalar amplitude of A s = 2.1 × 10 −9 [6] can be used to fix the parameter a at 1.66 × 10 −6 , which also controls the gravitino mass. Thus, the SUSY breaking scale (after inflation) is close to the inflationary scale in this class of models. Although the global U (1) R (g = 0) case is viable for inflation, it includes a massless R-axion, which motivates us to gauge the R-symmetry so that the axion is absorbed by the massive U (1) R vector, when the R-symmetry is spontaneously broken (an alternative would be to give mass to the axion by explicit R-symmetry breaking terms). In this case the gauge kinetic functions will be fixed by the requirement of anomaly cancellation via Green-Schwarz mechanism.
When the gauge coupling g is turned on, the requirement of viable inflation puts an upper bound on it of around g ∼ 0.8a 3 (no lower bound). This freedom to choose g can be used to control soft scalar masses to some extent. In Subsection 3.2 we will explore the allowed parameter space of this model in more detail.

Soft scalar masses
In our model defined by (1) and (2) (with general J) soft scalar masses are universal, where m 2 0 is given by and for the MSSM µ-parameter we assume |µ| |m 0 | to avoid extreme fine-tuning of the Higgs boson mass (since m 0 is close to the inflationary scale). From the requirement of (near-)Minkowski minimum, we have the relation, 4 The relation (17) allows us to rewrite m 2 0 in terms of the D-term contribution, and this leads to the requirement m 3/2 > κ D R / √ 2, in order to avoid tachyonic instabilities in the MSSM sector.
For the bilinear H u H d coupling we have where

Exploring the parameter space
In this subsection we analyze the parameter space of the model, namely the allowed values of the parameters α and β of the Kähler potential. We constrain the parameter space α − β by requiring (i ) stable Minkowski vacuum away from Z = 0, (ii ) concave potential (V ZZ < 0) around the origin for slow-roll hilltop inflation, and (iii ) non-tachyonic soft scalar mass, m 2 0 > 0 (see Eq. (18)). The parameter a can be factored out from the total scalar potential (thus determined by the scale of inflation), while the effective gauge parameter g/a is used as a variable in order to satisfy the requirements (i )-(iii ). The allowed parameter values are shown in Figure 1 as the blue shaded region. 5 In this allowed region we also compute the values of the spectral index n s : the orange dots represent n s > 0.954 (around 2σ values from CMB), and the red dots on the left-side represent n s > 0.9607 (1σ values). The effective parameter g/a varies from g/a = 0 (the line between blue and gray regions on the left) to g/a ≈ 0.75 in the allowed region. Although not shown in the plot, the effective parameter g/a is fixed at each point in the plot by the requirements (i)-(iii ), taking the values from 0 to ∼ 0.75.
As a concrete example we choose the following parameter values which leads to the inflationary parameters and the scalar potential depicted in Figure 2 where the non-canonical scalar Z is shown in blue, while the canonically normalized scalar z, found numerically, is shown in orange. The corresponding inflaton VEV is κZ = 0.89. We find that in the allowed parameter region, the smallest possible value of κZ compatible with a 2σ CMB constraint on n s is around 0.8, while 1σ values of n s favour κZ > 1.

Gaugino masses
The MSSM gaugino masses are generated at one loop via the Green-Schwarz mechanism of anomaly cancellation, where the gauge anomalies due to triangle diagrams involving the fermions (all the fermions of the model carry non-zero R-charges) are cancelled by appropriate U (1) R transformations of the following terms depending on the imaginary part of the gauge kinetic matrix, The gauge kinetic matrix of the model has the form, where f R,1,2,3 are gauge kinetic functions for U (1) R , U (1) Y , SU (2) L , and SU (3) c , respectively.
To cancel the anomalies we fix these kinetic functions as, where a = 1, 2, 3 stands for the Standard Model gauge groups. Here β are constants which we determine by using the methods described in Refs. [7][8][9]. The result is, where β R is found from the cancellation of The values of β a are the same as in the model of Ref. [3], because the MSSM fermions in the two models have the same R-charges, while β R is different due to the difference in the hidden sector fermion (inflatino) R-charges. Since g/κ in our models is not far from the Hubble scale (e.g. model I with the parameter choice (21) leads to g ∼ 10 −7 ), we have if κZ is around unity. Gauged U (1) R also leads to a gravitational anomaly which can be cancelled in a similar fashion (see for example Refs. [7][8][9]). This brings us to the MSSM gaugino masses, Using Eq. (26) we get, where we denote m a ≡ m aa . Finally, m a should be rescaled after taking into account noncanonical kinetic terms of the gaugini, However, if |β a | log κZ 1, as in the models that we consider here, the rescaling of the gaugini can be neglected.

Trilinear couplings
The trilinear couplings between the MSSM scalars are where for A 0 we have which is related to B 0 from Eq. (20) as A 0 = B 0 + m 3/2 (similarly to the model of Ref. [3]).

Soft parameters and mass spectrum
Here we show explicit values of the MSSM soft parameters for the parameter set (21), as well as the mass spectrum of the model. The results are summarized in Table 2, where we take one-loop values of the Standard Model gauge couplings 6 at the reheating temperature 10 8 GeV (estimated in the next subsection), As for the U (1) R gauge boson, its mass generated by the Higgs mechanism is 9.61 × 10 11 GeV, close to the inflaton mass. The parameters A 0 and B 0 are estimated as 1.25 × 10 12 6.15 × 10 11 7.51 × 10 11 2.68 × 10 11 1.03 × 10 10 6.54 × 10 9 5.84 × 10 9  As can be seen from Table 2, the inflaton mass is smaller than two times the gravitino mass, m z < 2m 3/2 , which prohibits the perturbative decay of the inflaton into gravitini. In order to see if this holds for other parameter values, we draw the ratio m z /(2m 3/2 ) as a function of α and β in Figure 3, showing that m z is smaller than 2m 3/2 in the relevant parameter range; due to the observed value of the spectral index, the relevant parameter region is constrained to a narrow strip around the lower limit of the allowed space, as shown in Figure 1. Therefore the inflaton-gravitino direct decay is forbidden. 7

Inflaton-MSSM interactions
Here we derive trilinear and quartic interactions between the inflaton and MSSM sparticles.
The first step is to find the inflaton |Z| in terms of the canonical inflaton which we call z. We define z such that z = 0. Although exact canonical parametrization may not be available (such as in our models), we only need to find the expansion of |Z| up to quadratic order in z. Let us denote dimensionless scalars as |κZ| ≡ ρ and κz ≡z, and expand ρ around the minimum, where the prime stands for d/dz. Derivatives of ρ can be found by requiring canonical normalization of the inflaton, This yields Then, any function f (ρ) can be expanded around the minimum (ρ = ρ which corresponds toz = 0) in terms of the canonicalz as follows (up to quadratic terms), where we used (36) and (38).
Using these results, we can derive the interactions of the inflaton with MSSM sparticles.
Trilinear scalar interactions The trilinear scalar interactions involving the inflaton are universal, and given by where the sum is over all MSSM scalars φ. We treat J as a function of ρ and introduce the notation also as a function of ρ. As can be seen the function h is dimensionless.
Quartic scalar interactions For quartic scalar interactions we have where Inflaton-gaugino interactions The trilinear inflaton-gaugino terms are given by where There is also the following inflaton-higgsino interaction, which is suppressed by κµ.
For model I with parameter set (21) the inflaton-MSSM couplings C φ , C a , d φ , andd φ have the values shown in Table 3.   (21).
Inflaton-inflatino interactions Since in our models SUSY is broken by both F -and D-terms, inflatino and gaugino mix with each other. In particular, the goldstino η is the following combination of fermions The physical fermion can be identified after choosing the unitary gauge η = 0. We can ignore the MSSM fields and use D R = g(κ −2 + J Z Z) and W = κ −2 aZ. Then, upon setting η = 0 in Eq. (48), we have which can be used to express the physical fermion orthogonal to the goldstino as ζ (or λ R ). The kinetic terms for ζ and λ R are given by where we used (49) and f R ≈ 1. Thus, for canonical normalization around the minimum we require The mass term of the physical fermion, as well as its trilinear coupling to the canonical inflaton z, can be derived from the following expression [5], where the terms with ∂ Z f R can be ignored since they are suppressed by g 2 (compared to other terms). Γ Z ZZ = J ZZ ∂ Z J ZZ is the Christoffel symbol for the Kähler metric J ZZ . To derive the mass term and relevant coupling, we use Eq. (49), the explicit forms of X Z R , D R , W , and the canonical normalization (51). Then Eq. (52) becomes where j is dimensionless. Finally, expanding j in terms of the canonical inflaton z by using Eq. (39) we find where ρ is the dimensionless non-canonical inflaton |κZ|, as before. The first term in (55) is the mass term of the inflatino m ζ = a j /κ which is 6.15 × 10 11 GeV for the parameter set (21), as we mentioned at the beginning of this section. The second term of (55) is the trilinear inflaton-inflatino coupling. For the parameter choice (21) its value is C ζ = 9.67 × 10 −8 .

Reheating
In model I the inflaton z can perturbatively decay into the MSSM scalars, gaugini, and inflatino since their masses are smaller than m z /2. The decay channels into MSSM scalars are given by Eqs. (40) and (42). In the quartic interactions the dominant contribution comes from the stop part due to its Yukawa coupling y t = O(1) (other Yukawa couplings are much smaller). Therefore the relevant terms for reheating are whereQ 3 is the third-generation quark doublet. Three-point (−σzϕ 2 ) and four-point (−λzϕ 3 ) decay rates for scalar particles (both z and ϕ real) are given by [13] ignoring the masses of the final-state particles (which can be justified in our case since the MSSM scalars are lighter than the inflaton roughly by a factor of ten). After including both real degrees of freedom canonically normalized as φ = (φ 1 +iφ 2 )/ √ 2 (z is already real canonical), the total decay rate into two MSSM scalars is where 49 is the number of species. The decay rate into three scalars comes from the second term of (56), which expands into three color and two weak components. In general, the product of three complex scalars plus its Hermitian conjugate reads, in terms of their real and imaginary parts, for example i.e. each individual quartic interaction of (56) contains four terms. Taking all of this into account, the total decay rate of z into three MSSM scalars (six relevant species) is given by where we take y t = 1 for simplicity. For the coupling with two fermions of the form 1 2 C λ zλ 2 + h.c., the decay rate is given by The values of the individual decay rates into gaugini and inflatino are shown in Table 4 where it can be seen that the decay into gaugini is negligible in comparison to the decay into inflatino. The total decay rate into fermions is then 2.86 × 10 −9 3.45 × 10 −9 7.25 × 10 −9 4.65 × 10 −4 Table 4: Inflaton decay rates (in GeV) into gaugini and inflatino for model I with parameter set (21).
From the total decay rate Γ tot = Γ tot z→φφ + Γ tot z→φφφ + Γ tot z→λλ = 6.54 × 10 −3 GeV , we can estimate the reheating temperature as, If we take other parameter values (α, β, g) from the allowed region in Figure 1, the mass hierarchy and the results for reheating may change, for example for the VEV of the inflaton is pushed to κZ = 1.2, and the observables are n s = 0.9631, r = 7.86 × 10 −5 (a is fixed as 1.56 × 10 −6 ). The corresponding mass spectrum is shown in Table 5. In addition, the U (1) R vector mass is 9.23×10 11 GeV. It can be seen that except for the inflatino and the U (1) R vector, all the masses are larger than in our previous parameter choice (see Table 2) but more importantly, the decay of the inflaton into MSSM scalars is kinematically forbidden, m z < 2m 0 , and the dominant contribution to the reheating temperature comes from MSSM gaugino decays. We found that the inflaton-gaugino couplings are larger in this case, which ultimately leads to a reheating temperature of the same order as before, at T reh ∼ 10 8 GeV.

Model II: hyperbolic Kähler space
The second inflationary model (with gauged R-symmetry) that we would like to consider is given by the Kähler potential [14] with two subclasses defined by γ = 2 and γ = 3, while δ is some real parameter which must satisfy |δ| 1 in order to describe slow-roll inflation (the parameters γ and δ are called α and β in [14], while our a is denoted by µ in that work). The superpotential for the inflaton is the same as before, W = aκ −2 Z, and the scalar potential of this model is given by As was described in [14], when δ = 0 we obtain no-scale de Sitter potential for γ = 2 and a 2 = 2g 2 , and for γ = 3 and a 2 = 9g 2 /2 (in both of these cases, the potential becomes constant and proportional to g 2 ). For realistic inflation we need a small deviation from these relations between a and g as well as a small non-zero |δ|. First let us fix γ. We find that when γ = 2, it is difficult to obtain positive squared masses for the MSSM scalars without extra scalars in the hidden sector. In particular we have, for the parameter sets described in [14]. On the other hand when γ = 3, the squared mass m 2 0 is positive even without extra scalars. To keep the field content minimal, we choose the γ = 3 case.
Next, as mentioned above, for γ = 3 we need a small deviation from δ = 0 and from a 2 = 9g 2 /2 in order to describe inflation. In particular, it is convenient to introduce a new parameter λ defined as a 2 = 9 2 g 2 (1 + λ) .
Then we require |δ| 1 and |λ| 1. Slow-roll inflation and stable Minkowski vacuum are possible along a specific trajectory in δ − λ space (with a and g fixed by the scale of inflationary perturbations). This trajectory can be seen in Figure 6 of Ref. [14].
Here as a specific example we take the following parameter values, 8 where the limit δ = λ = 0 leads to the no-scale case V = 2g 2 /κ 4 . The scalar potential for the parameters (70) is displayed in Figure 4 where we show both the non-canonical original scalar Z and the canonical one z (which is found numerically). In contrast to the previous model, here we always have positive m 2 0 in the allowed parameter space.
In this model the inflationary parameters are given by H = 9.38 × 10 12 GeV , n s = 0.9576 , r = 1.5 × 10 −3 , with the inflaton mass m z = 1.93 × 10 13 GeV, the vector mass m A = 1.1 × 10 15 GeV, and the inflatino mass m ζ = 1.1 × 10 14 GeV. Since we already derived MSSM soft parameters and inflaton-MSSM interactions for general J, here we just show the explicit results taking the parameter set (70). The mass spectrum is summarized in Table 6 and the values of the inflaton-MSSM coupling constants in Table 7.   Table 6: MSSM soft parameters (and the gravitino mass) derived from model II with parameter set (70). All the parameters are in GeV. The Standard Model gauge coupling values are taken at 10 8 GeV.
In our model II, MSSM scalars and inflatino are heavier than the inflaton, which means that the inflaton can only (perturbatively) decay into the gaugini λ 1,2,3 . The individual decay rates are 8Γ z→λ 3 λ 3 = 8.41 × 10 −2 GeV , and the total decay rate is Γ tot = 0.16 GeV. The reheating temperature is estimated as T reh 6 × 10 8 GeV.
As can be seen from Table 6, the gravitino in this case is much heavier than the inflaton, which prohibits the perturbative decay of the inflaton into two gravitini. In fact, this remains true for the whole parameter range that is suitable for realistic inflation, which can be seen as follows. In [14] it was shown that the scalar potential (for the canonical inflaton z) of model II in the aforementioned parameter range, can be approximated by the Starobinsky potential, which means that the inflaton mass is m z ≈ 8/3κ −1 g. Here g is our gauge coupling as before, which is related to a by (69), so that when |λ| 1 we have g ≈ √ 2a/3. On the other hand, the gravitino mass is given by m 3/2 = a e κ 2 J/2 |Z| . In the relevant parameter region the VEV of Z is | Z | ≈ κ −1 (for example for the parameter choice (70) we have | Z | ≈ 0.97κ −1 ), which leads to large VEV of J, where, again, |δ| 1. This implies that m z m 3/2 . More specifically, we find that in the relevant parameter space m z is smaller than m 3/2 by at least two orders of magnitude.

Modifications of Kähler potential
Unlike superpotential, Kähler potential in N = 1 theories is not protected from renormalization effects if they are allowed by symmetries of the model. In our case the local U (1) R symmetry allows for interaction terms between matter fields φ and the inflaton Z, as in the Kähler potential where ∆(ZZ) is an arbitrary function of ZZ. We take one matter field for simplicity, but for each one we can introduce a different invariant function ∆ i (ZZ).
Let us now examine the stability of the matter scalar potential in our models I and II, w.r.t. the modifications of the Kähler potential of the form (75). In particular, we want to make sure that the soft scalar mass squared, m 2 0 , remains positive at the minimum. Previously we found that m 2 0 can be expressed as (for general J-function) as found in Subsection 3.1. Once we take into account the ∆-term in the Kähler potential (75), this expression is modified as Therefore if ∆ ≤ 0, it cannot destabilize the φ = 0 vacuum (assuming we have m 2 0 > 0 in the absence of ∆). On the other hand, positive ∆ may introduce a tachyonic instability in φ-direction, if it is too large. This leads to the upper bound on the value of positive ∆ , which we call ∆ max , depending on a particular model and its parameters. For example in model I with parameter set (21) the upper bound is ∆ max ≈ 0.147. In model II with parameter choice (70) we find ∆ max ≈ 33.
Obviously, if MSSM scalars have distinct ∆-terms, this will lead to splitting between their masses,

Dark matter candidates
In both of the discussed models we have the mass hierarchy while the inflatino mass can be on either side depending on the parameter choice. On the other hand we assume that the parameter µ is much smaller than gaugino masses (for example from 100 GeV to TeV range) to avoid extreme fine-tuning of the Higgs boson mass. This leads to the so-called split Higgsino scenario [15] (see also [16]) where the two lightest neutralino states are Higgsino-like (the parameter µ corresponds exactly to the Higgsino Dirac mass term −µH uHd ). This makes the Higgsino-like LSP a potential candidate for the thermal cold dark matter if its mass lies within the TeV range. However, if µ is around the TeV scale, the huge difference between gaugino masses and µ suppresses the mass difference ∆m between LSP and next-to-LSP. This, in turn, may lead to inelastic scattering with nuclei which is constrained by direct detection experiments [17,18]. In Ref. [19] the authors showed that the lower bound on the mass difference ∆m 200 keV translates into the upper bound on the gaugino masses {m 1 , m 2 } O(10 7 ) GeV, if we assume that Higgsino-like LSP is the dominant part of dark matter. Therefore, as long as one persists in TeV scale µ, Higgsinolike LSP as the thermal dark matter is excluded in our models, because gaugino masses are much larger than the aforementioned upper bounds (the exception from this would be nonneutralino LSP scenarios, such as a hidden sector LSP or gravitino LSP, although the latter is not applicable to our models since our gravitino is generally too heavy). The overproduction of Higgsino dark matter also excludes a large window of its mass µ, from TeV scale all the way up to the reheating temperature (assuming standard thermal history), which in our case is at least 10 8 GeV.
If we give up the fine-tuning arguments and make µ as large as the SUSY breaking scale, LSP can become a candidate for superheavy dark matter [20,21] with mass m LSP ∼ 10 10 GeV. 9 In [20] it was shown that such heavy particles can be produced in sufficient amounts to describe dark matter, even if their mass exceeds the reheating temperature T reh , since the maximum temperature during reheating can exceed T reh by several orders of magnitude. Analytical approximation of the dark matter (denoted X) abundance in this case is given by [20] where α X ≡ m 2 X σ|υ| with σ|υ| the thermally averaged annihilation cross-section of X, m X is its mass, and g * is the number of relativistic degrees of freedom. Taking g * = 100, and requiring Ω 2 X h 2 0.3 (all dark matter is in X particles) we obtain a required value of the ratio T reh /m X , to produce the right amount of X dark matter. As can be seen, the result is not very sensitive to the annihilation parameter α X . For example as long as α X 10 −6 , the ratio is roughly T reh /m X ∼ 10 −3 . Let us assume that superheavy neutralino in our model I is one of the gaugini with the mass m X ∼ 10 10 GeV (see Table 2). Since the reheating temperature in this case is 10 8 GeV, this does not lead to the correct dark matter abundance (overproduction). It is however possible to obtain the correct ratio T reh /m X if we choose different parameters. For example the parameter choice (65) leads to a more suitable gaugino masses ∼ 10 11 GeV, as can be seen from Table 5, while the reheating temperature remains the same. We conclude that the parameter space in our models is flexible enough to accommodate superheavy LSP dark matter.

Discussion
In this paper we considered a class of single-field inflationary models defined by the gauging of U (1) R symmetry, and spontaneous breaking of supersymmetry and the R-symmetry after inflation where the goldstino is associated with a combination of inflatino and U (1) R gaugino. We focused on two subclasses of these models, which we call model I and model II, characterized by the geometry of the Kähler space. Model I has the canonical Kähler potential with higher-order corrections, while model II has hyperbolic geometry SU (1, 1)/U (1), also including corrections, where |Z| plays the role of the inflaton, while the phase of Z combines with the U (1) R gauge field to form a massive vector, with the mass close to the inflationary scale in model I, and far exceeding it in model II. The superpotential is fixed by the R-symmetry as W = aκ −2 Z. These models can describe slow-roll inflation with n s and r within 2σ CMB constraints (n s 0.954, r 0.064). For example for our reference parameter values (21) and (70), we have n s = 0.9543 and r = 1.72 × 10 −6 for model I, and n s = 0.9576 and r = 1.5 × 10 −3 for model II.
In both models the non-canonical inflaton |Z| takes sub-Planckian values, starting around |Z| = 0 and settling at | Z | < ∼ M P after inflation. This means that for small parameters α, β, δ in (82) and (83), we can treat the correction terms in the Kähler potentials as perturbations. On the other hand, the canonically normalized inflaton z travels sub-Planckian distances in model I (Figure 2), but super-Planckian distances in model II (Figure 4).
Having established the inflationary stage, we then coupled these models to MSSM according to Eqs. (1) and (2), and derived the resulting soft parameters and mass spectrum (shown in Tables 2 and 6). In this minimalistic approach, the scale of inflationary scalar perturbations fixes the scale of SUSY breaking, and therefore the scale of MSSM soft parameters. In particular, the universal soft scalar mass m 0 , as well as the scalar couplings A 0 and B 0 , are fixed at the tree level, while the gaugino masses are obtained after implementing Green-Schwarz mechanism for cancelling one-loop anomalies due to non-vanishing fermion R-charges. Our examples demonstrate that MSSM gaugino masses tend to be smaller than the MSSM scalar masses (for both models), but the mass hierarchy of the hidden sector fields (inflaton, inflatino, and the U (1) R vector) is model-dependent.
We derived the MSSM-inflaton couplings, and estimated the reheating temperature, generally T reh ∼ 10 8 GeV, from perturbative decay channels of the inflaton: in model I it can generally decay into all the MSSM sparticles, while in model II only gaugino channels are available kinematically. Our results also show that in the interesting parameter range of both models, the inflaton mass is smaller than two times the gravitino mass, which prohibits perturbative decay of the former into two gravitini. The full picture of reheating, however, requires further investigation after taking into account non-perturbative effects such as Bose condensation and possible resonant production of fermions.
We would like to point out that the R-charge assignment that we used in our examples (see the superpotential of Eq. (2)), where the MSSM scalars are neutral, is not the only possibility. Alternatively, we can assign R-charge of 1/2 to squarks and sleptons (in the convention where the superpotential has unit R-charge), while the Higgs scalars are neutral. In this case the quarks and leptons are neutral under U (1) R . Then, if the inflaton R-charge is one (same as before), we have the following superpotential, W = (κ −3 a +μH u H d )κZ +ŷ uū QH u −ŷ dd QH d −ŷ eē LH d .
Note that in contrast to our previous choice of the superpotential -Eqs. (2) and (3) -the inflaton Z does not couple to Yukawa terms here. This change of the superpotential does not significantly modify our results -the only part affected is the MSSM gaugino masses, as they depend on the number of R-charged fermions which has now been reduced. The consequence of this is that the gaugino masses become smaller, but by a factor of ten at most. Finally, we showed that our minimal models do not allow for thermal LSP dark matter, but superheavy LSP dark matter (e.g. neutralino) is possible depending on the parameter choice.

Appendix: Supergravity Lagrangian
We use notations and conventions of Ref. [5], except that we include the gauge couplings in the corresponding Killing vectors. The relevant part of N = 1 supergravity Lagrangian reads (M P = 1) for the bosonic sector, and e −1 L fermi = ε k mnψ kσ D m ψ n − e K/2 W ψ m σ mn ψ n + Wψ mσ mnψ n for fermions (h.c. applies to the second and third lines, and . . . stands for irrelevant terms such as non-renormalizable interactions). Here and D m acting on the fermions are appropriate Lorentz-/Kähler-/gauge-covariant derivatives.
The auxiliary F -field is eliminated via its equation of motion, while the D-field is equal to Killing potential D A (up to a minus sign) which is given by