On higher-spin supertranslations and superrotations

We study the large gauge transformations of massless higher-spin fields in four-dimensional Minkowski space. Upon imposing suitable fall-off conditions, providing higher-spin counterparts of the Bondi gauge, we observe the existence of an infinite-dimensional asymptotic symmetry algebra. The corresponding Ward identities can be held responsible for Weinberg’s factorisation theorem for amplitudes involving soft particles of spin greater than two.


Introduction and outlook
In this work we explore the possible relation between large higher-spin gauge transformations and soft theorems. Our main observation is that, upon imposing a reasonable choice of fall-off conditions at null infinity, the residual gauge transformations of Fronsdal fields [1] on a four-dimensional Minkowski background generate an infinite-dimensional Abelian symmetry algebra. The Ward identities of the latter, in their turn, can be shown to reproduce the factorisation formulae of Weinberg [2,3], in strict analogy with recent results concerning the asymptotic symmetry groups of spin one and spin two gauge fields [4,5].
Indeed, significant interest has been recently shown in the relation between two fairly old topics: asymptotic gravitational symmetries, discovered in the sixties by Bondi, Metzner and Sachs [6][7][8] and later reconsidered from various perspectives (see e.g. [9][10][11][12][13][14][15]), and soft theorems, i.e. relations among scattering amplitudes for processes involving the emission or the absorption of low-energy particles [2,3]. The explorations of the electrodynamical counterparts of this relation, involving the interplay between soft photons and large, spin-one gauge symmetries, pointed to the existence of a general underlying fieldtheoretical mechanism, thus adding further appeal to the subject. The main observation fostering the related ongoing activity is that Weinberg's soft photon and soft graviton theorems can be recast as Ward identities for suitably identified large gauge symmetries of electromagnetism and gravity, respectively [16][17][18][19].

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Weinberg's factorisation theorem, on the other hand, holds for soft massless particles of any spin, thus naturally leading to wonder which kind of asymptotic symmetry of the corresponding gauge theories, if any, may be held responsible for it. Our purpose is to try to elucidate this point, stressing the existence of an infinite-dimensional higher-spin symmetry algebra whose Ward identities can indeed be shown to reproduce Weinberg's result.
In section 2 we review and somehow rephrase the arguments concerning the structure of the asymptotic symmetry group for spin-two gauge fields, exploiting for our analysis solely the structure of the linearised theory. This allows us not only to introduce our notation and general line of approach, but also to propose a derivation of Weinberg's soft theorem where the equivalence principle has not to be assumed from the very beginning (rather, it is deduced), which is relevant in view of the extension to higher spins. In section 3 we consider a first class of large gauge symmetries of the Fronsdal action to be identified with properly defined higher-spin supertranslations. We determine the corresponding infinite-dimensional symmetry to then show how the associated Ward identities allow to derive Weinberg's soft theorem for arbitrary integer spin. Our construction is based on the definition of a suitable Bondi-like gauge for higher spins, whose consistency is further discussed in section 4. In section 5 we take a different perspective and consider the possibility to derive Weinberg's result for any spin as the Goldstone theorem of a specific class of large gauge transformations, thus extending the results of [20,21]. This approach provides a non-perturbative result that allows in principle to keep track also of the subleading corrections.
Higher-spin supertranslations are actually only a particular class of the transformations preserving our Bondi-like falloff conditions. We investigate the general form of the solution in section 6 (with some technicalities detailed in the appendices) with focus on the spin-three case, showing the existence of additional infinite families of asymptotic symmetries, providing proper higher-spin generalisations of superrotations [13,14,22]. The full structure of the asymptotic symmetry algebra for any value of the spin, the computation of the corresponding charges, together with a deeper assessment of its possible role and meaning, in particular in relation with the structure of subleading terms in soft theorems, will be explored in future work.
In our work we uncover a new class of infinite-dimensional symmetries. This is expected to improve our insight into higher-spin theories as knowledge of additional symmetries usually does. Weinberg's soft theorems, among other consequences, imply triviality of the amplitudes involving soft higher spin quanta. (See also [23] for a more recent analysis.) Still, we believe it to be hard to close the case concerning the relevance of massless higher spins in flat space until a clear connection with string amplitudes is established. The latter concern massive states, but it is expected that one could understand them as resulting from some massless phase with enhanced symmetry, arguably to arise after a properly defined tensionless string limit. (See e.g. [24] and references therein.) While this long-standing conjecture is usually addressed for symmetries that act everywhere in the space-time bulk, our work is meant as a first step in trying to extend the analysis at the boundary. Our ultimate hope is that these investigations may help to shed some light on the still largely mysterious infrared physics of higher-spin massless quanta.

JHEP05(2017)120 2 Soft gravitons and BMS symmetry
In [2,3], Weinberg showed that, using only the Lorentz invariance and the pole structure of the S matrix, it is possible to derive the conservation of charge and the equality of gravitational and inertial mass as consequences of the soft emission of the corresponding massless spin-one and spin-two quanta. On the same grounds, he argued that there can be no room for macroscopic fields corresponding to particles of spin three or higher. In short, Weinberg considered the S-matrix element S βα (q), for arbitrary asymptotic particle states α → β, also involving an extra soft massless particle of 4−momentum q µ ≡ (ω, q) → 0 and helicity s. The two main contributions to this process are schematically encoded in the following picture: + The second one, in particular, provides the leading contribution to the process and takes a factorised form that, in the notation of [2,3], can be written with η i being +1 or −1 according to whether the particle i is incoming or outgoing. To our purposes it is useful to rewrite Weinberg's result in terms of the so-called retarded Bondi coordinates (see e.g. [5]), where r = |x|. Consider now a wave packet for a massless particle with spatial momentum centred around q. At large times and large r, this wave packet becomes localised on the sphere at (null) infinity near the point so that the momentum of massless particles may be equivalently characterised by q µ or (ω, z,z). The polarisation vectors can be chosen as follows [25] ε where E i and (z i ,z i ) characterise the massless particles scattered to null infinity.

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For the case of spin 2, Weinberg's soft theorem has been recast as the Ward identity following from BMS supertranslation symmetry [5]. Moreover, it has been conjectured that infinitesimal BMS transformations provide a symmetry of both the classical gravitational scattering and the quantum-gravitational S matrix [4]. In particular, the Ward identity corresponding to this symmetry has been recognised to be the z-divergence of Weinberg's result (2.5) for s = 2, under the assumption that all gravitational couplings are equal (i.e. g (2) i ≡ 1), that is to say, assuming that the equivalence principle holds. Along an alternative path, one can infer the relevant Ward identity directly from the linearised theory via the quantum Noether theorem, as in the case of QED [19]. Let us go through this argument as well, so as to pave the way for our subsequent generalisation to higher spins. As an additional byproduct, we shall also be able to relate Weinberg's result to the Ward identities of supertranslations without assuming (rather, deriving, in a sense) the equivalence principle. In the following we shall make use of the coordinates (2.2).
The action for a massless Fierz-Pauli field h µν is where E µν is the linearised Einstein tensor Here and in the following a prime denotes a trace, while indices enclosed between parentheses are assumed to be symmetrised with the minimum number of terms needed and without normalisation factors. The Noether current associated to linearised diffeomorphisms, δh µν = ∂ (µ ν) , is By analogy with the non-linear, asymptotically flat case (see e.g. [5]), we consider the following form of h µν that we shall refer to as the "Bondi gauge", 1 to then look for the residual gauge freedom that keeps it. Notice that, by construction, h = 0. If, for simplicity, we restrict ourselves to gauge parameters µ which are u-independent and with power-like dependence on r we find a family of large gauge transformations parameterised by an arbitrary function T (z,z)

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on the celestial sphere, that we can write in two equivalent ways as follows: 2 where D z is the covariant derivative on the unit 2-dimensional sphere. In particular, the non-vanishing gauge variations are which represent infinitesimal BMS supertranslations. In this section we shall focus on these asymptotic symmetries. On the other hand, by allowing for the most general form of the residual gauge parameters (u, r, z,z) one recovers the full BMS algebra (see e.g. [14]): DzD · Y ∂z . (2.13) Indeed, the corresponding vector at I + spans an infinite-dimensional family of directiondependent translations parametrised by T (z,z), together with the transformations generated by the conformal Killing vectors on the sphere Y z (z) and Yz(z). From (2.8) we may now compute the leading contribution to the charge associated with the residual supertranslation gauge symmetry, where J(u, z,z) ≡ lim r→∞ r 2 J rr (u, z,z) . (2.15) We assume that supertranslations act on matter fields by δΦ(x) = iT (z,z)∂ u Φ(x) at I + and that this action is canonically realised by δΦ(x) = i[Q, Φ(x)], as shown in [4]. Analogous considerations apply to I − . The correlation functions therefore satisfy (2.16) 2 Recall δhµν = ∂µ ν + ∂ν µ − 2 Γ ρ µν ρ, where the Christoffel symbols for Minkowski space in Bondi coordinates are while γzz is the metric on the two-dimensional unit sphere.

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Performing the LSZ reduction of the previous formula yields the following Ward identity (for more details see [19]): where Q − denotes the counterpart of Q + at I − , and where f i depends in principle on i since we are not assuming that the gravitational couplings of each matter field be ruled by the equivalence principle. In analogy with [5], we now implement the auxiliary boundary condition Considering also that the matter current J acts trivially on the vacuum |0 , and hence it does not contribute to the left-hand side of (2.17), we effectively obtain Now, in order to drive our proof to conclusion, we propose the following choice for T (z,z): so that, using we can rewrite where the second term is a boundary contribution on the sphere and hence gives zero. Plugging this result, together with its counterpart at I − , into (2.17), one obtains (2.23) Performing the r → ∞ limit, so as to express C zz in terms of soft graviton creation and annihilation operators, one has Thus, using crossing symmetry, we also have out| ω a out + (ωx)|in = lim , (2.27) where we have used the divergence formula . (2.28) Note that we omitted the term proportional to ∂z 1 z−z i since here the delta multiplies a function which vanishes whenz =z i . This shows how the supertranslation Ward identity (2.23) implies Weinberg's factorisation formula (2.5), without assuming from the beginning f i = constant. 3

Higher-spin supertranslations
Owing to the fact that Weinberg's soft theorem holds for any spin, it is natural to wonder whether the corresponding factorisations for s ≥ 3 should be regarded as the consequence of some infinite-dimensional symmetries acting at null infinity, as for the electromagnetic and the gravitational cases. In this section, we provide an affirmative answer to this question. We first discuss the spin-three case, to then generalise our approach to the case of arbitrary spin. For more details on the ensuing construction see [27].

Spin three
Free spin-three gauge fields can be described by the Fronsdal action [1] with the "Einstein" tensor E µνρ given by where F is the Fronsdal, Ricci-like tensor: The action is invariant under the gauge symmetry with the gauge parameter constrained to be traceless: = 0.
3 Note also that our choice (2.20) of T (z,z) is not restrictive, since we can always write and use the linearity of the Ward identity to recover the full supertranslation symmetry from Weinberg's theorem.

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By analogy with the spin-two case, we choose our "Bondi-like gauge" near I + so that the following components are assumed to vanish while the other components scale in the following manner as r → ∞ where B, U z , C zz and B zzz are all independent of r, and we omitted subleading terms in r in (3.7). Analogous conditions hold for thez−components. Notice that by construction ϕ µ = 0. Let us stress that eqs. (3.5), (3.6) and (3.7) provide a combination of gauge-fixing and scaling behaviour at I + . Equivalently, one could set to zero only fewer components of the field using the off-shell gauge symmetry and fix suitable fall-off conditions on the others. The classification of asymptotic symmetries would then hold up to subleading undetermined contributions to the gauge parameter, corresponding to ordinary residual gauge symmetries. The consistency of our boundary conditions will be further discussed in section 4. Again, we ask ourselves whether there are residual gauge transformations, besides global Killing symmetries, leaving this structure invariant. The answer to this question is that there is indeed a residual gauge freedom given by the following family of tensors, parameterised by the arbitrary function T (z,z): while the corresponding contravariant tensor on I + is given by This residual symmetry generalises the gravitational supertranslations (2.10). In the remainder of this section we shall explore the link between higher-spin supertranslations and Weinberg's soft theorem, while postponing to section 6 the analysis of the full set of residual gauge symmetries of the Bondi-like gauge (3.5), (3.6) and (3.7). The non-vanishing gauge variations generated by (3.8) are:

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together with their conjugates. Like for s = 2, the only leading contribution to the Noether charge (a.k.a. surface charge) comes from δϕ zzz , and reads The surface charge thus computed is in agreement with that obtainable from the results of [28]. Under the assumption that the residual symmetry generators act on matter fields as follows, is the coupling of the corresponding matter field, in the frequency domain we get In addition, in close analogy with the condition (2.18) enforced in the spin-two case, we impose the auxiliary boundary condition at We also leave aside the J term, which again acts trivially on the vacuum, thus obtaining An analogous result holds for Q − . For the function T (z,z) we choose a slight modification of (2.20), (3.17) so that, after an integration by parts in ∂z, the computation of the charge involves where in particular the last term is a vanishing boundary contribution. To sum up: (3.20)

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The usual approximation for B zzz gives Thus, using crossing symmetry, we also have 23) and this implies, by comparing with (3.20), ( 3.25) This shows that the Ward identity of the residual spin-three gauge symmetry implies Weinberg's factorisation formula (2.5).

Spin s
This section is devoted to the generalisation of the previous results to arbitrary integer spin s. The Fronsdal action [1] is invariant under the gauge transformation with a traceless gauge parameter and a doubly-traceless field. Our Bondi-like gauge is summarised by the conditions ϕ rµ 2 ...µs = 0 = ϕ zzµ 3 ...µs (3.27) and for d = 0, . . . , s, together with their conjugates. These ensure in particular that the field be traceless: ϕ µ 3 ...µs = 0. The equations defining our residual gauge freedom, which are precisely those encoding the preservation of these scaling behaviours, are labelled by the following numbers: • the number p of "u" indices appearing, • the number d of "z" indices appearing withoutz counterpart, • the number c of pairs "zz", counted ignoring their order.

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For conciseness of notation, when useful, we shall also indicate by ϕ p d,c and p d,c the field components and the gauge parameter components, respectively, labelled with this counting criteria. The residual gauge freedom which preserves the given falloff conditions is independent of u, has power-like dependence on r and satisfies the trace constraint = 0. It admits the following parametrisation: where T p (z,z) for p = 0, . . . , s − 1 is a set of angular functions satisfying Therefore, this family of residual gauge transformations is defined recursively in terms of only one angular function T 0 (z,z) ≡ T (z,z). The non-vanishing gauge variations are, for s = p + d, which respect the r d−1 behaviour imposed on ϕ p d,0 . In particular the relevant contribution to the Noether current is given by Using the auxiliary boundary condition (D z ) s B z...zz = (Dz) s Bz ...zz and integrating by parts, the charge corresponding to our family of large gauge transformation is therefore where we have used the action

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on matter fields. The r → ∞ limit approximation gives Thus, Weinberg's factorisation can be understood as a manifestation of an underlying spin-s large gauge symmetry acting on the null boundary of Minkowski spacetime.

Consistency of the Bondi gauge
The Bondi gauge (2.9) is usually obtained from the fully nonlinear general-relativistic theory of asymptotically flat spacetimes. On the other hand, the falloff conditions on h µν can be seen to result from a choice of gauge in the linearised theory, together with the requirement that the field satisfies the equations of motion asymptotically, that is at leading order in an expansion in powers of r. Indeed, let us first impose the gauge-fixing condition h rµ = 0, and consider the field equations In particular, the equation for the component R rr in this gauge reads: Consider then the trivial solution: h zz = 0. The equation R uu = 0, taking into account the previous result, reads while R ru = 0 reads 2h uu

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Upon expanding h uu = 2m B r α + . . . and h uz = −U z r β + . . ., these equations yield at leading order 2 ∂ u m B r α−1 + ∂ u D z U z + DzUz r β−2 = 0 , Thus we see that the only choices avoiding unwanted constraints on the u dependence of m B and U z are either α = −1 and β = 0, or α = 1 and β = 2. We choose the "decaying mode" α = −1 and β = 0, thus obtaining Taking also into account the equation for the component R rz , i.e.
and substituting h zz = C zz r δ + . . . together with the other behaviours above, we have which imposes δ = 1 and All in all, we recovered the falloffs together with (4.6) and (4.9). One can also check that the equation R uz = 0 reduces to at leading order, and hence is identically satisfied in view of (4.9). One can similarly check that the remaining field equations are satisfied at leading order, consistently with the number of constraints imposed by the Bianchi identities. For the spin-three case, let us start by imposing ϕ µνr = 0, for µν = zz, which can always be achieved by exploiting the traceless gauge parameter µν . The equations of motion are Now, F rrr = 0 reads 2 which is consistent with ϕ rzz = 0. Similarly F µzz = 0 is solved by ϕ µzz = 0. Now, from F uur = 0 we have JHEP05(2017)120 and expanding ϕ uuu = B r α , ϕ zuu = U z r β , with β = α + 1, at leading order we have By comparison with F uuu = 0, which reads and yields, upon expansion, we have two possible behaviours: a "growing mode" α = 2, β = 3 and a "decaying mode" α = −1, β = 0. We choose the latter, obtaining ϕ uuu = B/r and ϕ zuu = U z , together with Which is solved by ϕ zzu = r C zz and Finally, from F zzr = 0, we have which gives ϕ zzz = B zzz r 2 and where for brevity ϕ ud denotes ϕ u...uz...z with d indices z and s − d indices u. Altogether these equations impose where the functions B d have to satisfy whereas the other equations are identically satisfied at leading order.

Soft quanta and Goldstone theorem
In two pioneering papers by Ferrari and Picasso [20,21], Weinberg's soft photon theorem [2] and its subleading corrections [29][30][31] were shown to follow from the Goldstone theorem applied to the breaking of a suitable class of "large gauge symmetries" of QED, namely those with linear gauge parameters. The photon itself was then reinterpreted as the associated Goldstone particle. In this section we generalise the strategy of [20,21] to all spins. In particular we detail the case of linearised gravity, since the higher-spin case obtains by the latter in a straightforward manner, as we sketch at the end of the section. For more details see [27]. We work in the harmonic gauge h µν (x) = j µν (x) , ∂ µ j µν (x) = 0 ; (5.1) here j µν (x) denotes the conserved stress-energy tensor of matter together with the nonlinear contributions from the Einstein equations in the ADM formulation [32]. The tensor j µν (x) also generates global space-time translations via the ADM energy-momentum tensor P µ . Consider the following family of infinitesimal local large gauge transformations, given by the linear gauge parameter µ (x) = − l µν x ν : where f denotes the coupling to gravity. Taking the vacuum expectation value of δ (l) h µν , we see that Therefore, since the transformation α(l) commutes with the dynamics and the vacuum expectations are not invariant under its action, it is a broken symmetry [33].
We turn now to the discussion of the implications of this spontaneous breaking on the spectrum of the theory. It is well-known that the breaking of an internal symmetry gives JHEP05(2017)120 rise to massless Goldstone excitations, but in the case at hand, α(l) does not commute with translations: indeed, denoting by τ (a) the action of infinitesimal translations, for a µ a constant four-vector, we see that We may therefore wonder whether the Goldstone theorem still holds. The answer to this question is affirmative: from the explicit form of the current which generates the large gauge transformations (obtained by the Noether theorem, using h µν = j µν and integrating by parts) we get One can extend the usual proof of Goldstone's theorem [21,33] by using the fact that the non-covariant piece of (5.6) involves the generator j µν = h µν of the (unbroken) global symmetry.
According to the Goldstone theorem, if the symmetry is broken then there are massless one-particle modes in the Fourier transform of 0|δ (l) B|0 , where B is the order parameter. More precisely where E 1 denotes the projection on zero-mass one-particle states while R and α refer to the appropriate test functions needed to give a well-defined charge. 4 Notice that the left-hand side of the previous equation is non-vanishing if and only if the symmetry is broken. Luckily, the non-covariant piece l µν x µ h ν0 gives no contribution to the right-hand side of (5.7) thanks to the spectral projector E 1 , which imposes k 2 = 0. Hence, we can write Noting that the Fourier transform of the integrand on the right-hand side is, by locality, an analytic function, we can once again rewrite this identity as follows: where Q µν R,α l µν = Q (l) R,α and The regulated charge is given by where the test functions fR and α satisfy

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taking also into account the Ward identity (5.13) when applying the derivatives on the right-hand side gives K µν (p, p , q) = i m j=1 Γ µν (p j , 0)S(p j ) + S(p j )Γ µν (p j , 0) K(p, p , q) The first line of (5.18) encodes Weinberg's poles as can be easily seen by considering, for instance, and is associated with those diagrams where the soft graviton is emitted or absorbed by an external line; the second line, on the other hand, encodes finite corrections corresponding to the other diagrams, analogous to those discussed for QED and gravity in e.g. [29][30][31]34] and [35]. The previous discussion can be naturally extended in the context of spin-s gauge theories, by choosing the higher-spin de Donder gauge, Limiting ourselves to the main formulae, the Ward identity linking the matter propagator S(p) to the s-field vertex function Γ µ 1 ...µs reads S(p)Γ µ 1 ...µs (p, 0)S(p) = − i s g (s) ∂ ∂p ρ η ρ(µ 1 p µ 2 . . . p µs) S(p) , (5.21) and the soft theorem expressing the amputated amplitude K µ 1 ...µs (p, p , q) for the process K(p, p , q) with the addition of an extra soft spin-s particle with momentum k µ is encoded in the following expression, Γ µ 1 ...µs (p j , 0)S(p j ) + S(p j )Γ µ 1 ...µs (p j , 0) K(p, p , q) . . p j µs) K(p, p , q) .

(5.22)
Let us stress that in close parallel to the low-spin case, also for spin s we obtain from the first line Weinberg's factorisation theorem for a spin-s soft particle, while the remaining terms encode subleading corrections, whose detailed analysis we postpone to future work.
6 Higher-spin superrotations: the spin-3 example In section 3 we identified asymptotic symmetries that suffice to recover Weinberg's factorisation theorem from the associated Ward identities. In this section we show that the full JHEP05(2017)120 set of residual gauge transformations leaving the boundary conditions invariant is actually much larger. Indeed, the additional symmetries are generated by a number of holomorphic and antiholomorphic functions, thus generalising the local infinite-dimensional enhancement of the Lorentz algebra observed in gravity [13,14]. For simplicity, we illustrate this phenomenon by focussing on a field of spin three. We generalise the Bondi-like gauge of section 3.1 and the analysis of asymptotic symmetries to any number of space-time dimensions. This approach allows to better appreciate how the infinite-dimensional enhancement appears to be a peculiarity of four-dimensional Minkowski space.

Boundary conditions reloaded
We parameterise the Minkowski background as follows: where γ ij denotes the metric on the unit celestial sphere of dimension n. The key of the Bondi-like gauge proposed in section 3.1 lies in the choices The number of conditions that one imposes in this way is the same as in the transversetraceless gauge, which is reachable on shell for any value of the spin. Therefore we assume that the conditions (6.2) can be imposed for any n on field configurations satisfying Fronsdal's equations asymptotically (as the gravity Bondi gauge does) and that possible deviations are suppressed at null infinity so as to become irrelevant for the analysis of asymptotic symmetries. 5 The power-like radial dependence of the remaining components -specified in (3.7) when the dimension of space-time is equal to four, that is for n = 2 -is such that ϕ uuu shares the same leading exponent as the one of the deviation h uu from the background metric in gravity, while the other leading exponents grow by one unity for any additional angular index on the celestial sphere. As shown in section 4, these conditions guarantee that the fields satisfy the linearised equations of motion at leading order. Following the same reasoning, one can generalise (3.7) as follows: where, in order to satisfy (6.2), the tensors C ij and B ijk are bound to be traceless,

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The falloff of ϕ uuu corresponds to the "standard" falloff of h uu in asymptotically flat solutions of higher-dimensional gravity [26,36]. 6 As detailed in appendix A, fields behaving in this way at null infinity solve Fronsdal's equations at leading order in an expansion in powers of r for any value of n, 7 provided that the following relations hold: where D i denotes the covariant derivative on the celestial sphere. The previous discussion formally applies also to odd space-time dimensions, which the analysis of [26,36] does not encompass, while in the special n = 2 case the first relation in (6.5) is substituted by the weaker condition (4.18), involving a u-derivative of the same tensors. Analogy with the gravitational falloffs and consistency with the linearised field equations are our main motivations for imposing the boundary conditions (6.2)-(6.5), where one could also adopt a conservative viewpoint and bound the value of n to be even in analogy with [26,36,37]. 8 We are now going to identify the residual gauge transformations leaving them invariant.

Higher-spin superrotations
The conditions δϕ rµν = 0 fix the radial dependence of all components of the traceless gauge parameter µν . The first three conditions in fix instead the dependence on u. All in all, the previous constraints, together with the constraint g µν µν = 0, are satisfied by Alternative boundary conditions for gravity -designed to keep supertranslations also when the dimension of space-time is larger than four -have been proposed in [37]. A similar option may be foreseen for higher spins too; we postpone an analysis of this issue to future work. Here we employ boundary conditions affine to those usually considered in literature for gravity, implementing the idea that fields should falloff faster at infinity with the increasing of the dimensionality of space-time. 7 In complete analogy, the boundary conditions that give finite higher-spin charges in AdS also satisfy the field equations asymptotically [38,39]. In three space-time dimensions these falloffs have also been proved to remain valid even when interactions are switched on [40]. 8 In three space-time dimensions, asymptotic symmetries for higher-spin fields in Minkowski space have been studied in the Chern-Simons formulation [41,42], while the relation between I ± ∓ has been studied in [43]. Our fall-off conditions (6.3) differ from the metric-like translation of the Chern-Simons boundary conditions displayed in [42]. To gain a better grasp on possible subtleties emerging when the number of space-time dimensions is odd, it will be interesting to analyse how the proposal of [42] may fit into the previous discussion.

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Before presenting the corresponding radial components, let us stress that the key point of the whole analysis is that the residual symmetry is parameterised by the tensors T (x k ), ρ i (x k ) and K ij (x k ) defined on the celestial sphere. They appear at O(r 0 u 0 ) respectively in uu , ui and ij and they must satisfy some differential constraints that will be specified below. The combinations T ij A (K), U ij A (ρ) and V ij 2 (T ) -where the subscript denotes the order of the differential operators involved -are instead displayed in appendix B. The tensors T , ρ i and K ij completely specify also the radial components of the gauge parameter as follows: where A i (K) and B i (ρ) are given in appendix B. Gauge parameters of this type induce variations of the fields such that δϕ rµν = 0 and δϕ uuu = 0, while δϕ uij = r 2 2(n + 1) D·R ij − u r (n + 1)(n + 2) D (i D j) + 2 γ ij ( + 2(n + 1)) D·ρ − r 6n D·T ij , (6.14) where we introduced the traceless tensors

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We recall that, as in previous sections, indices enclosed between parentheses are assumed to be symmetrised by using the minimum number of terms needed and without normalisation factor. Consistently with the analysis of section 3.1, when n = 2 the boundary conditions (6.2)-(6.5) are preserved by gauge transformations generated by an arbitrary function T , while ρ i and K ij must satisfy When n > 2, these constraints still apply, while with our choice of boundary conditions T also has to satisfy T ijk = 0 .
Moreover, the identities (B.8)-(B.10) guarantee the preservation of the boundary conditions when n > 2, by ensuring the cancellation of the terms that cannot be anymore interpreted as variations of U i , C ij and B ijk . Notice also that, consistently with the relations (6.5) induced by the requirement that the linearised field equations be satisfied at leading order, when n = 2 one has 0 = ∂ u D i δU i , (6.23) The characterisation of asymptotic symmetries therefore reduces to the classification of the solutions of the equations (6.19) (plus (6.20) when n > 2). First of all, let us stress that, for any value of n, these equations must admit a number of independent solutions that is greater than or equal to the number of traceless rank-2 Killing tensors of Minkowski space. In Cartesian coordinates, the latter indeed satisfy the equations ∂ (µ νρ) = 0 , g µν µν = 0 , (6.26) which are just a particular instance of the problem at stake and are solved by where the involved tensors are traceless and irreducible, that is A (µν|ρ) = A (µν|ρ)σ = 0. This implies that (6.26) admit n(n+3)(n+4)(n+5) 12 independent solutions. When n > 2, solving either (6.6) or (6.26) actually imposes the same conditions on the gauge parameters. In appendix B we also verify explicitly that the number of solutions of (6.19) and (6.20) agrees with that of (6.26), at least when one considers the flat limit of the former.
On the contrary, when n = 2 the function T (x k ) is not constrained at all if one only demands preservation of the Bondi-like gauge. This leads to the higher-spin supertranslations discussed in section 3.1. The tensors ρ i and K ij are instead still bounded to satisfy the differential equations (6.19). Remarkably, when n = 2, locally they both admit infinitely many solutions. This is well known for the first equation in (6.19), which is the rank-2 conformal Killing equation [44]. Being traceless, it only admits two non-trivial components that, using a holomorphic parameterisation of the metric, read Its solutions are therefore locally characterised by a holomorphic and an antiholomorphic functions: In a similar fashion, the second traceless equation in (6.19) only admits two non-trivial components that one can cast in the form These equations are solved by where k(z,z) is the Kähler potential for the 2-dimensional metric on the unit sphere. For instance, in the coordinates (2.2) one has k(z,z) = 2 log(1 + zz). α(z) and β(z) are instead arbitrary holomorphic functions and similar considerations apply to the antiholomorphic sector.
To conclude, we wish to sketch a possible interpretation of the infinite-dimensional families of symmetries we found. In the case of gravity supertranslations can be considered as an infinite-dimensional enhancement of the Poincaré translation symmetry generated, say, by P i . Similarly, superrotations correspond to an infinite-dimensional enhancement of the Lorentz symmetry generated by M ij . As discussed in appendix B, the global solutions of the constraints (6.19) and (6.20) are in one-to-one correspondence with the traceless projections of the combinations P (i P j) , P (i M j)k and M k(i M j)l . After a proper specification of the involved representation, these products are expected to be identified with the spin-three generators of a would-be higher-spin algebra, if any, with Poincaré subalgebra (see e.g. [45,46] for discussions on higher-spin algebras possibly related to four-dimensional Minkowski space). The asymptotic symmetries generated by T , ρ i and K ij can thus be interpreted as the infinite-dimensional enhancement of the Killing symmetries associated, respectively, to the products of Poincaré generators P (i P j) , P (i M j)k and M k(i M j)l . Certainly, controlling better this relation will require to consider interactions, in order to JHEP05(2017)120 capture possible non-Abelian deformations of the asymptotic symmetry algebra. Let us anyway notice that, up to the signature, the M ij also generate the algebra of isometries of AdS 3 . Their products -or, more precisely, a proper quotient of the universal enveloping algebra of the Lorentz algebra -should then give a subalgebra isomorphic to one of the AdS 3 higher-spin algebras that appeared in the literature. The latter are generically asymptotically enhanced to W-symmetries [47][48][49][50], which are generated by the conformal Killing tensors of the two-dimensional boundary of AdS 3 [40]. The compelling similarity with the symmetry generated by K ij suggests that any possible non-Abelian deformation of our algebra of asymptotic symmetries should contain an infinite-dimensional non-linear W-algebra as a subalgebra.

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Finally, the component with all indices valued on the celestial sphere reads +r (r∂ r +(n−2))D (i ϕ jk)u +2 γ (ij D l ϕ k)lu −2 r 2 (r∂ r +(n−1)) γ (ij ϕ k)uu . (A.7) An ansatz of the form Eq. (A.7) gives instead so that the corresponding equation of motion is satisfied at leading order if α = −n/2 (which avoids the restrictive condition ∂ u B ijk = 0 having no analogue in gravity). This leads to the fall-off conditions considered in section 6. When n > 2 the equations of motion associated to (A.1)-(A.3) are then satisfied at leading order provided that Imposing these conditions, the equations of motion associated to (A.4)-(A.6) are satisfied as well at leading order, consistently with the number of constraints imposed by the Bianchi identities (which is equal to the number of independent components in F rrr , F rru , F rri , F uuu , F uui and in the identically traceless F uij ). The case n = 2 is special also in this respect, since the equation F ruu = O(r α−3 ) is identically satisfied for α = −1 thanks to the factorisation of (α + 1). As discussed in section 4, in this case one should look at which gives the weaker relation ∂ u B = ∂ u D i U i instead of the first condition in (A.13).

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B More details on the residual gauge symmetry In this appendix we display the differential combinations of the tensors T , ρ i and K ij that we omitted in section 6 when presenting the structure of the gauge parameters generating asymptotic symmetries. We also display the identities that allow to fully express the variations (6.14) and (6.15) in terms of the differential constraints K ijk , R ijk and T ijk when n > 2. Finally, we show that the number of solutions of (6.26) coincides with that of (6.19) and (6.20), at least when solving the latter in their flat limit.

Gauge parameters
The tensors entering the expansion of ij in (6.7) are The tensors entering the expansion of ri in (6.10) are

Gauge variations
The variations δϕ uij and δϕ ijk displayed, respectively, in (6.14) and (6.15) contain some terms that have not been rewritten in terms of the differential constraints (6.19) and (6.20). This reflects the existence of non-trivial variations of the boundary data in n = 2 under both higher-spin supertranslations and superrotations. 9 On the other hand, when n > 2, compatibility with the falloffs (6.3) requires that these residual variations vanish. This is guaranteed by the following identities: γ (ij D k) (3 +2(n−1)) D·ρ Note the overall factors (n − 2) in the left-hand sides, which still allow for non-trivial variations in four space-time dimensions.

Differential constraints
Let us now turn to the equations (6.19) and (6.20). For simplicity, we evaluate their number of independent solutions by analysing them in the flat limit, assuming that the dimension of the solution space remains the same, as it is manifest for the equation K ijk = 0, which is only rescaled under Weyl rescalings of the metric. We therefore consider the equations The different relative factors with respect to (6.16)-(6.18) are induced by our convention for the symmetrisations, since ∂ (i ∂ j ρ k) contains e.g. less terms than D (i D j ρ k) because ordinary derivatives commute. When n > 2, eqs. (B.11)-(B.13) are solved by x k x l +ω ij|k x k x 2 +c kl 4 x i x j x k x l −4 ν k (i x j) x l x 2 +δ i k δ j l x 4 , (B.14) ρ i = a i +λ x i +b ij x j +ω i|j x j +ã i x 2 +c j x i x j +Ω jk|i x j x k +λ x i x 2 +ω i|j x j x 2 where all tensors in the solutions are traceless and irreducible. As a result, the number of integration constants is T ∼ (n + 1)(n + 4) 2 , ρ i ∼ n(n + 2)(n + 4) 3 , K ij ∼ (n − 1)(n + 2)(n + 3)(n + 4) Open Access. This article is distributed under the terms of the Creative Commons Attribution License (CC-BY 4.0), which permits any use, distribution and reproduction in any medium, provided the original author(s) and source are credited.