Higuchi Bound on Slow Roll Inflation and the Swampland

In this paper we study the implications of the generalized Higuchi bound on massive spin-two fields for the derivative of the scalar potential within bimetric theory. In contrast to the recent de Sitter swampland conjecture, an upper bound on the derivate of the scalar potential follows from the generalized Higuchi bound. In combination, this leaves a window for the derivate of the scalar potential. We discuss this bound in several representative bimetric models and parameter regions.

In this paper we study the implications of the generalized Higuchi bound on massive spin-two fields for the derivative of the scalar potential within bimetric theory. In contrast to the recent de Sitter swampland conjecture, an upper bound on the derivate of the scalar potential follows from the generalized Higuchi bound. In combination, this leaves a window for the derivate of the scalar potential. We discuss this bound in several representative bimetric models and parameter regions.

I. INTRODUCTION
As it is extensively discussed during the recent two years, the effective potential of scalar fields in effective gravitational theories is severely constrained by fundamental quantum gravity or string theory considerations [1][2][3][4][5][6]. These constraints have profound implications on the evolution of the universe, in particular on inflationary scenarios and on the problem of dark energy [7,8].
A genuine feature of quantum gravity and string theory is the existence of higher spin fields. The effective field theory of higher spin fields is highly constrained. One such constraint is the Higuchi bound [9], for a massive (bosonic) field of spin s and mass m that propagats in de Sitter (dS) spacetime with radius 1/H (with H the Hubble parameter). If the bound is violated the massive higher spin field contains helicity modes with negative norm which is in conflict with unitarity. Recently some implications from the Higuchi bound on massive higher spin states in string theory and on the scale of inflation were discussed in [10,11]. The Higuchi bound is non-trivial for s ≥ 2. In this article we focus on massive spin-2 fields [12,13] with Fierz-Pauli mass m FP . Here the Higuchi bound explicitly reads m 2 FP ≥ 2H 2 . In the case where the Hubble parameter is given by the potential energy of a scalar field, i.e. 3H 2 = V , the Higuchi bound provides an upper limit on the potential energy as given the mass of the spin-2 field. In Ref. [14] the Higuchi bound of dS spacetime was generalized for FLRW spacetime to a cosmological stability bound. This bound was found in the context of bimetric * mlueben@mpp.mpg.de † dieter.luest@lmu.de theory [15,16] which serves as the low-energy effective field theory for a massive and a massless spin-2 field with fully non-linear (self-)interactions. In section III we examine implications of this bound in bimetric theory for the derivative of the scalar potential, denoted by V . In contrast to the swampland condition of [2], where a lower bound on V is conjectured, we will show that an upper bound on V follows from the generalized Higuchi bound.

II. INGREDIENTS FROM BIMETRIC THEORY
In order to describe a massive spin-2 field propagating on a curved background such as FLRW, the linear theory by Fierz and Pauli [12,13] must be completed by nonlinear terms [17,18]. Bimetric theory is the ghost-free non-linear completion of Fierz-Pauli describing a gravitating massive spin-2 field [15,16,19,20]. For a review we refer to Ref. [21]. Furthermore, for some work about bimetric theory in relation to the swampland and string theory realizations see [22][23][24][25][26].

A. Action and equations of motion
We focus on singly-coupled bimetric theory where the Standard Model couples to only one of the metric tensors, say g µν . The action for the metric tensors g µν and f µν is given by [15] where R(g) and R(f ) are the Ricci scalars of g µν and f µν , resp. The quantity M p is the Planck mass of g µν and α = M f /M p measures its ratio to the Planck mass of f µν . The bimetric potential is defined in terms of the square-root matrix S µ α S α ν = g µα f αν (or in matrix notation S = g −1 f ) and given by β n e n (S) (4) in terms of the elementary symmetric polynomials e n . The parameters β n are real and have mass dimension 2 in this parametrization. Note that β 0 and β 4 parametrize the vacuum energy in the g µν -and f µν -sector, resp. Finally, Standard Model fields are collectively denoted as Φ.
Varying the action (3) with respect to g µν and f µν yields two sets of modified Einstein equations, where G g µν and G f µν are the Einstein tensors of g µν and f µν , resp. The explicit form of contributions coming from the bimetric potential U g µν and U f µν can be found, e.g., in Ref. [15,27]. The stress-energy tensor of matter is defined as If the matter-sector √ −gL m is invariant under diffeomorphisms, stress-energy is conserved, ∇ µ T µν = 0, where ∇ µ is the covariant derivative compatible with g µν . The Bianchi identity ∇ µ G g µν = 0 implies the so-called Bianchi constraint

B. Proportional background solutions
An important class of solutions are the proportional backgrounds where both metric are related by a conformal factor, f µν = c 2 g µν [28]. The Bianchi constraint forces c to be a constant. These solutions are maximally symmetric, i.e. (A)dS or Minkowski. The effective cosmological constant in terms of the bimetric parameters is given by The equality of the first and second line follows from the proportionality of the Einstein tensors for g µν and f µν .
Here, we already anticipated that the matter sector contributes potential energy V to the effective cosmological constant. Therefore Λ is composed out of vacuum energy, interaction energy of the massive spin-2 fields, and potential energy from the matter sector. Eq. (8) can be thought of as determining the proportionality constant c.
Bimetric theory has a well-defined mass spectrum around proportional backgrounds. The metric fluctuations are a linear superposition of mass eigenstates. The mass of the massive spin-2 field is given by in terms of the bimetric parameters. We refer to this quantity as Fierz-Pauli mass. As mentioned previously, the Fierz-Pauli mass is subject to the Higuchi bound [9], to ensure unitarity.

C. Flat FLRW solutions
Assuming homogeneity and isotropy according to the cosmological principle, both metrics are of FLRW from [29][30][31], Here, the functions a and b are the scale factors of g µν and f µν , resp, while X is the lapse of f µν . All metric functions depend on time t only. We introduce the Hubble rate H and the scale factor ratio y as where a dot denotes derivative with respect to cosmic time t.
Next, we assume that the matter sector consists of a real scalar field φ with Lagrangian with scalar potential V (φ). According to the cosmological principle, the scalar field can only depend on time t. Consequently, the energy density and pressure are given by The stress-energy tensor is given by The equation of motion for the scalar field reads Next, we derive the Friedmann equations. The Bianchi constraint is solved by on the so-called dynamical branch 1 . Plugging the ansatz (11) into the modified Einstein eq. (5) yields two sets of Friedmann equations. These can be rearranged to give a single Friedmann equation. Here, we adopt the notation of Ref. [34] where the Friedmann equation reads in terms of the time-varying effective Planck mass The function U depends on the parameters of the bimetric potential as The scale factor ratio is determined by a quartic polynomial, where the polynomial P (y) is given by in terms of U with U = dU/dy. The consistency of the solutions to this equation have been studied in detail in Refs. [35][36][37]. However, in this note we will adopt a perturbative treatment.

D. Generalized Higuchi bound
By inspecting the sign of the kinetic term of the scalar mode in the minisuperspace approximation, the authors of Ref. [14] derived a cosmological stability bound that generalizes the Higuchi bound to FLRW spacetime. Let us define a time dependent mass parameter as This quantity reduces to the Fierz-Pauli mass (9) when the metrics are proportional 2 , i.e. for y = X = c. It was shown that the kinetic term of the scalar mode is multiplied by The kinetic term of the scalar mode has the correct sign if This is the generalized Higuchi bound that we will use in the next section. Note, that this bound reduces to the standard Higuchi bound when the metrics are proportional.

III. CONSTRAINT ON THE DERIVATIVE OF THE SCALAR POTENTIAL
As mentioned previously, the Higuchi bound provides an upper limit on the (local) minimum of the scalar potential. By studying small displacements from the minimum, we now derive a bound on the derivative of the potential close to its minimum. We will work in the slow-roll approximation. We assume that Λ V , i.e. the potential energy of the scalar field dominates over the vacuum and interaction energy. We further assume that the Higuchi bound is not saturated, i.e. we exclude the partially-massless case [38,39], in order to avoid devision by zero.
First, we express the energy density of the scalar field in terms of the potential V and its derivative. Let us introduce the slow-roll parameter where V means derivative of V with respect to the scalar field φ. In the slow-roll approximation 1 andφ Hφ, the scalar equation of motion (16) can be rearranged toφ Replacing H using the Friedmann eq. (18) and eq. (14) yields after rearranging Solving forφ yieldsφ 2 = −V (1± 1 + 4 /3) out of which only the '−' branch is physical (as only thenφ = 0 for = 0). Plugging this back into our expression for the energy density, yields up to first order in slow-roll. Plugging this into the Friedmann equation yields Here we used that M eff /M p ∼ O(1) during slow-roll. To find an expression for the generalized spin-2 mass m gen up to first order in slow roll we plug eq. (29) into the quartic polynomial (21) and solve for y order by order in . This results in Here, c is the solution for = 0, i.e. at the de Sitter point where the cosmological constant is given by the potential energy of the scalar field only. The Fierz-Pauli mass is defined on that background as in eq. (9). Plugging this into eq. (23) yields up to first order in slow-roll. The quantity F depends in the bimetric parameters and scalar potential as The expression in parenthesis does not combine into welldefined background quantity. Combining our ingredients, we find W in the slow roll approximation as For F ≥ 2V /3 the bound on is trivial. However if the Higuchi bound is satisfied and if F < 2V /3, we find the following non-trivial bound on : In appendix A we discuss typical values of the right hand side of eq. (34) by studying various simplified models and different regions of the parameter space. We generally find that the right hand side is of the order of m 2 FP /V . That means, if the mass of the spin-2 field is close to the Higuchi bound, the restriction on V is most stringent as we assumed slow-roll to start with.
Finally, the bound (34) implies for the derivative of the scalar potential, Here we used again that generally M eff /M p ∼ O(1). Hence, we found an upper limit on the derivative of the scalar potential. The restriction is most stringent close to the Higuchi bound. Saturation of the bound is excluded and hence the right hand side cannot vanish.

IV. SUMMARY AND DISCUSSION
We used bimetric theory as the low-energy effective field theory to describe a massive spin-2 field with mass m FP propagating on FLRW spacetime. Assuming that the matter sector is composed out of a scalar field with potential V , we showed that the generalized Higuchi bound implies an upper bound on the slow roll parameter of the following form: For the derivative of the scalar potential an equivalent upper bound can be written as In our derivation we assumed that only the potential energy of the scalar field contributes to an effective cosmological constant. For a large spin-2 mass m 2 FP V , this bound is not restrictive as we assumed slow-roll (i.e. 1) in our derivation. On the other hand, if the mass of the spin-2 field is close to the Higuchi bound, the derivative of the scalar potential is bounded from above.
Let us compare our result with the bounds on the scalar potential, which are obtained in the context of the de Sitter swampland conjecture [2,4], stating that with c , c being some universal constants of order one. This bound rules out de Sitter vacua and restricts slow roll inflationary scenarios in string theory. Applying the lower bound from the de Sitter swampland conjecture and combining it with the upper bound from the generalized Higuchi bound in bimetric theory, it follows that the derivative of the scalar potential has to lie in the following window: The window is small when the spin-2 mass is close to the Higuchi bound, in which case the derivative has to be of the order |V |/V 1/M p . However, due to the Higuchi bound, the window does not close completely. Let us point out some caveats again. The Higuchi bound on V was found within the slow-roll approximation. Further, there are specific parameter regions where V is not bounded from above. However for generic parameters, the bound in eq. (39) on V applies.
In string theory it is natural to assume that the spin-2 mass m FP is related to higher spin string excitations. Assuming that eq. (37) holds generally and identifying the spin-2 mass with the string scale, m FP M s , our bound reads Here g s is the string coupling constant, and V denotes the internal volume of the compact six-dimensional space. We can use the bound on M s that was obtained in Ref. [10], which follows when one requires that the entire string Regge trajectory satisfied the Higuchi bound. So taking also this bound into account, the condition (40) is always satisfied if the following stronger bound holds: As a next step it would be interesting to study whether the upper bound on V is a generic implication of unitarity when massive spin-2 fields propagate on dS spacetime. This requires a treatment beyond slow-roll. Further, it would be interesting to check, wether this combined bound is satisfied, e.g., in concrete string theory settings.
In this section, we provide explicit expressions for the upper bound on in terms of the background variables m FP and V for several representative bimetric models and parameter regions. The relation between the interaction parameters and the background quantities was studied in detail in Ref. [37]. Note that in general, the bimetric potential gives rise to an effective cosmological constant Λ. Here, we assume that only the scalar potential contributes to the overall cosmological constant, i.e. we assume Λ V . In the following, we only state the results and point out some caveats about the more restricted submodels. For brevity, let us define the maximum value of as in terms of which the generalized Higuchi bound in slowroll approximation reads < max . First we discuss models with only two non-vanishing interaction parameters. For the β 0 β 1 -model, defined by setting β 2 = β 3 = β 4 = 0, we find Note that the β 0 β 1 -model is only well-defined for m 2 FP > V which is more restrictive than the Higuchi bound. For spin-2 masses in the range V < m 2 FP < 10 9 V the bound on is trivial because 01 max < 0. Expanding around m 2 FP V the expression simplifies to 01 max 3m 2 FP /V . Setting β 0 = β 2 = β 3 = 0, we find for the β 1 β 4 -model Therefore, close to the Higuchi bound the restriction on is most stringent. For the β 1 β 2 -and β 1 β 3 -model, the explicit expression for max is lengthy. Instead, we only state their values in the limit m 2 For both models the bound on epsilon is trivial in the large mass limit. To summarize, in fig. 1 we plot max as a function of the spin-2 mass and the scalar potential for the 2 parameter models. We see that within the β 1 β 3 -model and β 1 β 4model the small mass limit implies max 1. Hence, in this parameter region the bound is non-trivial. In that case, the bound on scales like ∼ m 2 FP /V . Next, we study more general cases by moving to 3 parameter models. For convenience, we introduce the quantityᾱ = αc [37]. We demonstrate the bound for the β 0 β 1 β 4 -model (blue) and the β 1 β 2 β 3 .model (red) in fig. 2 as a function of m 2 FP /V for different values ofᾱ. As a general behavior we find that max O(1) or negative in the limit of smallᾱ. Moving away fromᾱ 1 the upper limit on scales like max ∼ m 2 FP /V for both models. For the β 1 β 2 β 3 -model the value of max is additionally suppressed by inverse powers ofᾱ in the limitᾱ 1. However this parameter region is excluded by consistency conditions [37]. To summarize, in the consistent parameter region we find the same order of magnitude for max as for the 2 parameter models.
Finally, we move to the full bimetric model with all interaction parameters left free. Solving the background eqs. (8) and (9) we can replace the interaction parameters β 1 , β 2 , and β 3 in terms of the physical parameters m FP , Λ = V , andᾱ = αc. We also introduce the quantityβ 4 = α −4 β 4 . In terms of these parameters, the upper limit on reads Although this expression is quite lengthy, we can discuss the order of magnitude for different parameter regimes.
In the limit of a large mass, m 2 FP V , while keepingᾱ finite, the expression reduces to The pre-factor involvingᾱ is always of order 1 (i.e. for small and for large values ofᾱ). Next, we expand max for small (GR-limit) and for large (massive gravity limit)ᾱ resulting in In both limits, the order of magnitude is set by m 4 FP /(β n V ) and suppressed by (inverse) powers ofᾱ. However, this conclusion is model-dependent. In our parametrization the interaction parameters β 0 andβ 4 are fixed, while the other parameters scale withᾱ in a nontrivial way. We also studied the limit of small and largē α in other parametrizations. We find that max is not necessarily suppressed by (inverse) powers ofᾱ, while in these cases the order of magnitude is set by m 2 FP /V . Summarizing, there are regions of the parameter space where the bound on is trivial either because max 1 or because max < 0. However, as the typical value we find max m 2 FP /V . Therefore, close to the Higuchi bound the limit on the gradient of the scalar potential is most stringent.