Massive spinning bosons on the celestial sphere

A natural extension of the Pasterski-Shao-Strominger (PSS) prescription is described, enabling the map of Minkowski space amplitudes with massive spinning external legs to the celestial sphere to be performed. An integral representation for the conformal primary wave function (CPW) of massive spinning bosons on the celestial sphere is derived explicitly for spin-one and -two. By analogy with the spin-zero case, the spinning bulk-to-boundary propagator on Euclidean AdS is employed to extend the massive CPW integral representation to arbitrary integer spin, and to describe the appropriate inverse transform of massive spinning CPWs back to the plane wave basis in Minkowski space. Subsequently, a massive spin-s momentum operator representation on the celestial sphere is determined, and used in conjunction with known Lorentz generators to derive Poincaré symmetry constraints on generic massive spinning two-, three- and four-point celestial amplitude structures. Finally, as a consistency check, three-point Minkowski space amplitudes of two massless scalars and a spin-one or -two massive boson are explicitly mapped to the celestial sphere, and the resulting three-point function coefficients are confirmed to be in exact agreement with the results obtained from Poincaré symmetry constraints.


Introduction
Minkowski space scattering amplitudes can be equivalently mapped to the celestial sphere at light-like infinity, where they are encoded in terms of conformal correlator objects called celestial amplitudes. This map for amplitudes of massive scalars and massless particles of various spin was described by Pasterski, Shao and Strominger (PSS) [1,2]. Ideally, the goal is to discover so called Celestial Conformal Field Theories (CCFT) that would give rise to celestial amplitudes for specific scattering processes of interest, entirely from the celestial sphere perspective without reference to Minkowski space amplitudes. While to this date no example of a CCFT is known, note that since the map to the celestial sphere is bijective, celestial amplitudes can also be considered more pragmatically as a new basis for the original Minkowski space amplitudes. Alternative descriptions of scattering amplitudes can potentially reveal hidden features that were not previously accessible from other points JHEP06(2020)079 of view. Considering that asymptotic states that serve as input to scattering amplitudes originate at or near the celestial sphere, investigation of an amplitude description entirely on this boundary without reference to the bulk of Minkowski space is particularly interesting.
In [25] we have derived the explicit constraints on celestial amplitudes implied by Poincaré symmetry (based on conformal Ward identities and momentum conservation), making use of the representation of Lorentz and massless momentum generators on the celestial sphere [12]. Considering that conformal primary wave functions and the map to the celestial sphere for amplitudes involving spinning massive particles have not been discussed in the literature to date, the constraints presented in [25] omit the case of spinning massive particles. In this work we set out to fill in these gaps, and obtain the following results.
In the massive case, we take the Ansatz that the plane wave basis functions of an entire spin multiplet are to be mapped to the celestial sphere collectively, instead of a single spin component value in the direction of propagation. This is well motivated by the fact that a single spin value in direction of propagation is not a conserved quantity under Poincaré transformations, while on the other hand the entire multiplet transforms into itself. Demanding the appropriate transformation properties on the celestial sphere, we determine the explicit integral representation for spin-1 and -2 massive conformal primary wave functions (CPW) by solving differential equations derived from a Lorentz transformation infinitesimally close to the identity. The integral representation is in line with the massive scalar case discussed in [1]. By analogy with the scalar case, we point out that the integration weight in the integral representation of the massive conformal primary wave function of arbitrary spin is given by a respective bulk-to-boundary propagator on Euclidean Antide Sitter space H 3 . This relation also reveals a straightforward inverse transform of the massive conformal primary wave function back to Minkowski space, based on an integral over the split representation of a harmonic function known in the literature [30].
A natural extension of Pasterski-Shao-Strominger (PSS) prescription, to enable the map of Minkowski space amplitudes with massive spinning external legs to the celestial sphere, follows directly from the conformal primary wave function discussion by recalling that amplitudes are multi-linear in polarization tensors, such that the polarization part of the integration weight for the integral transform hides within the amplitudes.
With the integral representation of the massive conformal primary wave function in hand, we derive a corresponding massive momentum operator representation on the celestial sphere, which has the appropriate momentum eigenvalue in the bulk. The resulting momentum operator turns out to be spin dependent and non-diagonal in spin multiplet space. As required, this momentum operator properly closes the Poincaré algebra, which proves that it is indeed correct for arbitrary integer spin s.

JHEP06(2020)079
Making use of this newly discovered massive spinning momentum operator representation, we repeat the analysis of [25] and derive the explicit constraints on two-, three-and four-point structures implied by conformal Ward identities and momentum conservation in the case when massive spinning external particles are present.
In the two-point case we find that the resulting recurrence relations for the two-point function coefficient can be solved. However, as in the massive scalar case [25], the Mellinlike integral in the inverse transform to Minkowski space diverges, such that there is no corresponding two-point amplitude counterpart in Minkowski space.
In the three-point case with two massless and one massive particle we show how the three-point function coefficient for the entire spin multiplet of the massive particle can be built up iteratively. The expected property that the difference of helicity values of the two massless particles produced in the decay of a massive particle may not exceed the maximum spin that can be accommodated by the spin multiplet of the massive particle, emerges as a multiplet truncation condition from the celestial sphere perspective.
Generically, the momentum conservation constraints admit three-point function coefficient solutions that allow for periodic dependency on individual conformal dimensions ∆ = 1 + iλ of the external particles. As we discussed in detail at the end of section 4 in [25], periodic holomorphic functions of finite order are unbounded on any complex vertical line, which spoils the convergence of the Mellin-like integration over −∞ < λ < ∞ in the inverse transform back to Minkowski space. To ensure convergence, the three-point function coefficient better have no non-trivial periodicities in ∆ i .
In three-point cases with two massive and one massless particle, or three massive particles, as well as the four-point case with one massive and three massless particles, we report the explicit resulting recurrence and differential equations for three-point function coefficient and four-point function of conformal cross ratios. While these equations are hard to solve in general, they are likely to be useful as consistency requirements when working with specific amplitude examples on the celestial sphere.
Finally, as a cross check, we perform the map of tree-level amplitudes of two massless scalars and one massive spin-1 or -2 particle from Minkowski space to the celestial sphere. We find the expected three-point function coordinate dependence, and the resulting threepoint function coefficients perfectly agree with our results obtained purely from symmetry. This work is organized as follows. In section 2 we recall the problem setting, introduce spinning massive conformal primary wave functions and demonstrate their inverse transform back to the plane wave basis in Minkowski space. In section 3 we present the spinning massive momentum operator representation on the celestial sphere. Section 4 investigates the explicit constraints implied by conformal Ward identities and momentum conservation on two-, three-and four-point structures involving massive spinning particles. Appendix A parametrizes massive spin-1 and -2 polarization tensors, appendix B discusses the formalism of encoding symmetric transverse traceless tensors in terms of polynomials, while appendix C shows examples of three-point Minkowski space amplitudes mapped to the celestial sphere.

JHEP06(2020)079
2 Spinning massive conformal primary wave functions 2.1 On-shell massive and massless momentum parametrization in the bulk As described in [1], the mass-shell of a massive momentum vector is parametrized by a hyperbolic slice of Minkowski space. This H 3 slice in Poincaré coordinates y, z,z has the metric and features the SL(2, C) isometry Such an H 3 slice asymptotes to the so called celestial sphere at the boundary y → 0. The SL(2, C) transformations on H 3 entail Möbius transformations of complex coordinates w,w on the celestial sphere, which involve the same transformation parameters: The embedding of a mass m on-shell ((mp) 2 = −m 2 ) momentum into Minkowski space while a massless (light-like (ωq) 2 = 0) momentum pointing to a point on the celestial sphere amounts to the vector with an energy scale ω. This parametrization satisfies the constraint We work with a projection of the celestial sphere onto a complex plane C, which has the metric 1 while the inverse bulk metric can be expressed as Note that the parametrization of q µ actually produces an induced metric of a complex plane on the boundary. Equivalently, we could work with an induced metric of a complex sphere instead, if we redefine ω → ω 1+ww , such that q µ effectively receives an extra factor 1 1+ww .

Map of spinning massive amplitudes to the celestial sphere
The map of Minkowski space amplitudes A n with massless external particles of various spin to celestial amplitudes A n on the celestial sphere at light-like infinity has been derived in [2] to be given by the Mellin transform in the energy scale ω j of the j-th massless external particle momenta in an appropriate polarization gauge. Here, the leading ellipsis denote suppressed transforms for potentially present massive particles, to be discussed below. Parameters λ j enter the conformal operator dimensions in continuous series representation, so that particle properties are encoded by operator insertions on the celestial sphere. Since massless particles reach specific points at light-like infinity directly, their helicity values l j map diagonally to the spin values J j of corresponding operator insertions. For the case of external massive scalar particles in a Minkowski space amplitude, the map to celestial amplitudes was obtained in [1], for each j-th massive external scalar, to be given by where the leading ellipsis denote suppressed transformations for other types of external particles in A n . The integral transformation weight (−q j ·p j ) −∆ is the so called scalar bulk to boundary propagator on H 3 [30]. The integral transform collects contributions from the entire mass shell y j , z j ,z j and returns a localized insertion point w j ,w j on the celestial sphere for j-th external scalar. It is our objective to generalize this mapping prescription to accommodate the cases of massive spinning external particles.

JHEP06(2020)079
Recall that amplitudes in Minkowski space are multi-linear in polarization tensors of external particles (2.14) with as many sets of s j Lorentz indices on the uncontracted amplitude as there are massive spinning particles with polarization tensors b i involved in the process. 2 The subscripts b i are spin (in direction of propagation) multiplet indices for the massive particles.
Considering that a Lorentz transformation in the bulk can flip the spin component along the axis of propagation of a massive particle, it is natural to propose that an amplitude of definite spin particles on the celestial sphere is to be obtained from a combination of all spin component values of the respective spin multiplets in the bulk. Therefore, we seek a map where each massive external leg of an amplitude is transformed to the celestial sphere as . . , s i . The leading ellipsis denote suppressed integral transforms for possibly present massless particles (2.11), which are unchanged.
In the next subsection we describe how the integration weight matrix G (s i ) J i b i can be obtained from the consideration of spinning massive conformal primary wave functions.

Spin-zero, -one and -two massive conformal primary wave functions
As defined in [1], the conformal primary wavefunction of a mass m scalar (outgoing/ incoming: ±) on the celestial sphere can be obtained via the integral transform of the plain wave basis in Minkowski space analogously to (2.13). In this section we set up an ad-hoc procedure to obtain the mapping of the massive spin s plain wave basis Guided by our expectation of how amplitudes involving spinning massive particles are to be mapped (2.15), we seek an integration weight matrix G In [2], conformal primary wave functions φ were defined as solutions to the massive Klein-Gordon equation with appropriate covariant transformation properties. The ansatz (2.18) trivially satisfies the Klein-Gordon equation, since all plane waves do. Here we exploit the fact that the integration weight matrices G (s) Jb are uniquely fixed (up to row normalization) by demanding appropriate covariant transformation properties, which fixes the integral representation of φ.
The desired conformal primary wavefunction φ must transform as a conformal primary on the celestial sphere, and maintain the usual Lorentz transformation Λ µ ν on the Minkowski vector indices. The exponential and the integration measure in (2.18) are invariant under such transformation, so that the combination of integration weight matrix and polarization tensors must transform as Requiring this transformation property, we may consider a Lorentz transformation (2.10) that is infinitesimally close to the identity: with α, β, γ infinitesimal, and similarly forā,b,c,d andᾱ,β,γ. Taking as a convenient ansatz G (s) Jb , using known expressions for the polarization tensors (e.g. (A.1) and (A.3) for spin-one and -two respectively) and expanding (2.19) to linear order in the infinitesimal transformation parameters, yields a set of coupled first order differential equations in w,w, z,z, y variables for the matrix components g (s) Jb , which can be easily solved iteratively.
In cases of spin-zero, -one and -two this procedure straightforwardly gives

JHEP06(2020)079
where the (2s + 1) × (2s + 1) matrix components are labeled by indices J, a ∈ {−s, . . . , s}, and where we have chosen a particular normalization for each row that will be convenient for the parametrization of the massive momentum operator representation discussed in the following section. The integration weight matrices above can be written more succinctly by introducing the following building blocks With this, the spin-1 integration weight matrix is given by while the spin-2 integration weight matrix amounts to Note that a G (s) Ja µ...ν a conveniently simplifies and is equal to the above expressions with the complex conjugate polarization factors * aµ 1 ...µs dropped.

Arbitrary integer spin massive conformal primary wave functions
While the procedure in the previous section is useful to develop conceptual understanding and investigate a few explicit examples of lower spin, it is too cumbersome to parametrize the arbitrary spin situation. Luckily, by analogy with the fact that the scalar integration weight (−q ·p) −∆ in (2.16) is the scalar bulk-to-boundary propagator on H 3 , the product of integration weight matrices with polarization tensors a G (s) Ja µ...ν a is also related to spinning bulk-to-boundary propagators on H 3 . More precisely, we start with spin-|J| bulkto-boundary propagator [30] (dropping a normalization factor): where I µν is one of the building blocks in (2.24). Y µ and Z µ are auxiliary variables encoding tensor structures on the H 3 (p 2 + 1 = 0) slice and the light cone (q 2 = 0) respectively, which are discussed in appendix B. Sincep µ I µν = 0 = I µν q ν , expression (2.27) satisfies transversality on both sets of indiceŝ To obtain an object that transforms as a R 1,3 spin-s Lorentz tensor, we take the (s−|J|)-fold formal derivative Y · ∇p = Y · ∂p:

JHEP06(2020)079
where the prefactor is inserted for later convenience, and (a) n = Γ(a+n) Γ(a) is the Pochhammer symbol. Subsequently, as outlined in appendix B.2, we use the operator R µ defined in (B.14) to recover the symmetric traceless transverse tensor encoded by the polynomial in auxiliary Z µ variables. The action of (Dq · R) |J| facilitates a contraction of Dq µ vectors with the symmetric traceless transverse tensor indices, which (up to normalization) effectively reduces to replacing each Z µ by Dq µ , as outlined in (B.20), (B.21). Finally, we take the plus or minus spin component pull-backs to the celestial sphere with a convenient coefficient, which leads to the definition where θ x = θ(x) is the Heaviside step function, and As discussed in appendix B, a transverse symmetric and traceless tensor with s Minkowski indices is then recovered by applying the special differential operator (B.3) s times in succession. This directly produces the product of integration weight matrix with polarization tensors, discussed in the previous sub- This demonstrates that the map to the celestial sphere is properly invertible, and the spinning massive conformal primary wave functions form a complete basis.

Spin-s massive momentum representation and Poincaré algebra
As already seen in the massive scalar case [25], massive momentum operators on the celestial sphere are spin dependent. In fact, since a definite spin conformal primary wave function for a massive particle mixes all the spins in the bulk multiplet (2.18), the massive spin-s momentum representation on the celestial sphere is simultaneously a Minkowski vector, as well as a matrix in spin multiplet space 4 Ja of the spin-s massive conformal primary wave function (2.18). Each component µ of the operator P µ J,I turns out to be a non-diagonal matrix in spin multiplet space, and we found it to be explicitly given by: Note that since only δ J,I+1 , δ J,I , δ J+1,I are involved, only neighboring spins are coupled. 4 The same is formally true in the massive scalar case, where P µ J,I with µ = 0, 1, 2, 3 and J, I = 0.

JHEP06(2020)079
Since the normalization of each row in the integration weight matrix G (s) Ja can be chosen separately, the off-diagonal terms of the massive momentum operator depend on this normalization as well. The result (3.3) is designed to specifically match the row normalization for all J explicitly chosen in (2.32).
It is straightforward to explicitly verify that this momentum operator indeed satisfies the defining equation (3.2), e.g., for s = 0, 1, 2, 3 making use of (2.32). Additionally, it is easy to analytically verify that it properly squares to −m 2 K η µν P µ J,K P ν K,I = −m 2 δ J,I , for arbitrary integer spin s ≥ 0. All Lorentz generators M µν J,I = −M νµ J,I are diagonal in spin multiplet space (see [12]) where ∂ x = ∂ ∂x . The Lorentz algebra can be written with spin multiplet indices made explicit where η µν is the mostly plus Minkowski metric. The momentum operator P µ J,I then completes the Poincaré algebra [M µν , P ρ ] = K M µν J,K P ρ K,I − P ρ J,K M µν K,I = i η µρ P ν J,I − η νρ P µ J,I , [P µ , P ν ] = K P µ J,K P ν K,I − P ν J,K P µ K,I = 0 . (3.11) The proof that (3.3) indeed is a correct (general spin s) massive momentum operator representation on the celestial sphere, is due to the fact that it squares to −m 2 as pointed out in (3.4) and properly closes the Poincaré algebra (3.11) for arbitrary integer spin parameter values s ≥ 0, which can be straightforwardly verified analytically. The massless momentum representation for any spin s is given by [12] P µ J,I = δ J,I q µ e ∂ ∆ , (3.12) which is diagonal in helicity space, same as the Lorentz generators M µν J,I , so that in the massless case the Poincaré algebra closes for each helicity independently and the spin multiplet indices can be suppressed.

JHEP06(2020)079 4 Poincaré constraints on massive spinning celestial amplitudes
As in the case of celestial amplitudes involving massive scalars [25], Lorentz symmetry constraints, with i labeling the scattering particles from 1 to n: . . δ Jn,In A I 1 ,...,In = 0 (4.1) with summation over each −s j ≤ I j ≤ s j for j = 1, 2, . . . , n implied, are equivalent with conformal covariance of primary field correlator structures in CFT, so that the shape of each structure can be fixed to the following familiar form 5 [28,29] (4.2) where in the two-point case we use Dirac and Kronecker deltas to keep ∆ 1 , ∆ 2 and J 1 , J 2 formally apart (which is required, since momentum operators act on particles 1 and 2 separately), and we use the conformal weight abbreviations Further constraints on the two-and three-point function coefficients C and the function of cross-ratio f are expected to result from momentum conservation requirements . . δ Jn,In A I 1 ,...,In = 0, (4.7) where i = ±1 for particle i incoming/outgoing, and summation over each −s j ≤ I j ≤ s j for j = 1, 2, . . . , n is implied. In the following we systematically derive the resulting constraints.

Two-point structure
The two-point structure is special due to the presence of the delta functions δ(∆ 1 − ∆ 2 )δ J 1 ,J 2 . Application of the massive momentum operators in the equation i i P i µ A = 0 leads to four independent delta function combinations that cannot cancel each other. 5 Here and throughout the paper we sometimes use abbreviations xij ≡ xi − xj for various quantities with particle indices.

JHEP06(2020)079
On the support of δ(1 + ∆ 1 − ∆ 2 )δ J 1 ,J 2 we have the constraint where we use the abbreviations ∆ 2 = ∆ + 1, ∆ 1 = ∆ and J 1 = J 2 = J. While, on the support of δ(−1 where we use the abbreviations ∆ 2 = ∆ + 1, ∆ 1 = ∆ and J 1 = J 2 = J. To reconcile these two equations we must take m 1 = m 2 = m , s 1 = s 2 = s , (4.10) while 1 = − 2 is required by kinematics. Without loss of generality we rescale the twopoint function coefficient as such that the constraint above implies the periodicity of c J ∆ under ∆ → ∆ + 1. Making use of this ansatz, the two remaining constraints on the support of δ( Considering that J is integer, this equation has a known explicit recurrence solution. Formally reintroducing the distinction between ∆ 1 and ∆ 2 as well as J 1 and J 2 , the general solution for the two-point function coefficient can be summarized as where c x is periodic under x → x+1, and we kept the spin multiplet number s 1 = s 2 = s the same. In case s = J 1 = J 2 = 0 this readily reduces to the scalar result found in [25]. Note that, as discussed in [25], in order to avoid convergence issues in the inverse integral transform back to Minkowski space, c x better be trivially periodic (ergo constant). However, again as in the scalar case [25], even without periodicities the inverse transform to Minkowski space is not defined, since the Mellin-like integration over ∆ 1 = ∆ 2 = ∆ = 1 + iν with −∞ < ν < ∞ directly hits a pole at ν = 0 in the (pseudo-) scalar contribution of the multiplet J 1 = J 2 = J = 0. Therefore, even though a non-trivial two-point celestial structure exists, its map to Minkowski space is not well defined. This is consistent with the fact that there is no non-trivial two-point amplitude in Minkowksi space. The two-point function coefficient for a two-point structure of one massless and one massive particle is constrained to vanish, same as in the scalar case.

Three-point structure
In the three point case we can consider amplitudes involving one, two, or three massive external particles, while the remaining particles are massless. The case when the massive particles are scalars has been investigated previously [25]. In this section we repeat the analysis for massive particles of non-zero spin.
Two massless, one massive. When one of the three particles is a spinning massive boson, the equations i i P i µ A m,0,0 = 0 lead to four independent constraints, which can be expressed symmetrically in indices 2 and 3 for overall upper and lower cases of the double-signs as: 6 All four of these recurrence relations involve three different terms with non-diagonal parameter shifts which makes this system of equations hard to solve in general. However, note that one of the two equations (4.15) reduces to two-term recurrence relations with shifts in the parameter ∆ 1 only, in the case when J 1 = s 1 or J 1 = −s 1 respectively. With this it is possible to make progress as follows. If we start, e.g., with the highest weight J 1 = s 1 , then without loss of generality we choose to rescale the respective three-point function coefficient as where, kinematically, only the incoming-outgoing combination 1 = − 2 = − 3 makes sense. With this, the upper sign equation in (4.15) reduces to implying that c must be periodic under ∆ 1 → ∆ 1 + 2. Using this, the equations (4.14) with J 1 = s 1 simplify to

JHEP06(2020)079
As explained in appendix B of [25], this implies that ∆ i dependence in c must either appear in combination i ∆ i (in which case it must be periodic under i ∆ i → i ∆ i + 2 due to periodicity of ∆ 1 ), or else must be periodic under ∆ i → ∆ i + 1. For the same reason as discussed at the end of section 4 in [25], assuming on physical grounds that c is a holomorphic function of finite order, a non-trivial periodicity of c makes it unbounded on any complex vertical line in the complex plane. Therefore, to ensure convergence of the inverse integral transform of the celestial amplitude back to Minkowski space, c better be trivially periodic -ergo constant. 7 The ansatz (4.16) as well as the periodicities of c can then be used in the lower sign equation in (4.15) to iteratively generate C s 1 −l,J 2 ,J 3 ∆ 1 ,∆ 2 ,∆ 3 for l = 1, 2, . . . , 2s 1 in terms of the initial J 1 = s 1 expression. The iteration must truncate after l = 2s 1 steps, at which point the J 1 spin multiplet is complete. A factor of (J 1 + s 1 ) in (4.15) ensures that no further C J 1 −1,J 2 ,J 3 ∆ 1 ,∆ 2 ,∆ 3 term is generated once J 1 = −s 1 ; however, the rest of the terms in this equation must then cancel exactly for the multiplet truncation to be consistent. Explicitly generating multiplets for a few s 1 values such as s 1 = 1, s 1 = 2, or s 1 = 3, reveals that the rest of the terms in the J 1 = −s 1 truncation equation does not cancel automatically, but instead becomes proportional to The consistency requirement of the multiplet truncation therefore implies that the difference of helicity values of two massless particles produced in the decay of a massive particle may never exceed the maximum spin that can be accommodated by the spin multiplet of the massive particle 8 Naturally, we can start with J 1 = −s 1 and build up the multiplet in the opposite direction instead. In that case the role of eqs. (4.15) with upper and lower signs is reversed, but all multiplet construction steps proceed analogously. In appendix C we consider explicit examples of three-point amplitudes with two massless scalars and one massive spinning external particle mapped to the celestial sphere. There we find exact agreement with the three-point function coefficient obtained above purely from symmetry, with c trivially periodic in conformal dimensions c s 1 ,J 2 ,J 3 ∆ 1 ,∆ 2 ,∆ 3 = const.
One massless, two massive. When two of the three particles are spinning massive bosons, the equations i i P i µ A m 1 ,m 2 ,0 = 0 lead to four independent constraints, which 7 Considering ∆i = 1 + iλi, the ratio of gamma functions in (4.16) vanishes as 1/λ1 for λ1 → ±∞ and as e −π|λ j |/2 for λj → ±∞ with j = 2, 3. Therefore, even the first non-trivial periodic mode e 2πin∆ in a Laureant expansion of an integer-periodic holomorphic function would dominate the suppressing effect of the gamma function ratio and must therefore be ruled out. 8 Compare with section 4.1 in [32].

JHEP06(2020)079
can be expressed symmetrically in indices 1 and 2 as: where in (4.22) the index combination i = 1, j = 2 is taken together with the upper of the double-signs, and combination i = 2, j = 1 is taken with the lower of the double-signs.
Zero massless, three massive. When all three particles are spinning massive bosons, the equations i i P i µ A m 1 ,m 2 ,m 3 = 0 again lead to four independent constraints. One constraint can be given as: where (cyclic) denotes terms with indices 1, 2, 3 cyclically interchanged. The remaining three constraints can be summarized as (abbreviating C = C J 1 ,J 2 ,J 3 ∆ 1 ,∆ 2 ,∆ 3 ): In case when the massive particle is a scalar s 4 = J 4 = 0, these equations properly reduce to the constraints found in [25].
Two massless, two massive and beyond. As in the massive scalar case [25], for the four-point structure, momentum conservation always leads to four constraints which consist of coupled shift equations in conformal dimensions of the four-particles, while simultaneously being differential equations in conformal cross ratios. In the massive spinning case, shifts in spins of massive particles also occur. When two or more massive particles participate, the resulting four equations similarly can be straightforwardly generated from the application of momentum operators to (4.4), but are quite unwieldy. Therefore, we do not spell these equations out explicitly.

JHEP06(2020)079
Acknowledgments We thank F. Denef, C. Sleight and M. Taronna for interesting discussions. We are especially grateful to A. Joyce for in-depth conversations and useful suggestions throughout the course of this project. AL and MZ are supported by the US Department of Energy under contract DE-SC0011941.
A Spin-one and -two massive polarization tensors Spin of massive particles is encoded by polarization tensors (compare this section, e.g., with section 2.2 in [33]). In the spin-1 case the polarization vectors of spin a = −1, 0, +1 describing circular polarizations in the plane perpendicular to momentum mp µ are parametrized as which satisfy all required polarization properties: Higher spin polarization tensors generically can be composed out of the spin-1 polarization vectors given above by taking appropriate symmetric and traceless combinations. For instance, in the spin-2 case the a = −2, −1, 0, +1, +2 components read such that once again all required polarization properties are satisfied: µν ap ν = 0 , * a µν bµν = δ a,b , 2 a=−2 * a µν a ρσ = 1 2 P µρ P νσ + 1 2 P νρ P µσ − 1 3 P µν P ρσ , where P µν = η µν −p µpν p 2 , and µν a η µν = 0 for each index a by construction.

B Polynomial encoding of symmetric traceless transverse tensors review
In this appendix we review the formalism of encoding symmetric traceless transverse tensors in terms of polynomials of auxiliary variables [31].

JHEP06(2020)079
As explained in [31], the information of an STT tensor is fully encoded by this polynomial if the following restrictions are imposed on the auxiliary variable Y : We think of the polynomial (B.1) as living on this sub-manifold. To extract the original STT tensor from H(p, Y ), we use the differential operator which acts interior to (B.2), i.e. for any arbitrary function g(Y ) we have Additionally, it is easy to verify that the operator is symmetric, transverse and traceless and therefore its action on any polynomial of Y defines a transverse traceless symmetric tensor on (B.2). The original tensor can be recovered from the polynomial via where (a) n = Γ(a+n) Γ(a) is the Pochhammer symbol. To take formal derivatives of an STT tensor with respect top µ , we use the covariant derivative operator which acts interior to the submanifold (B.2), and transverse (p · ∇p = 0). This satisfies Y · ∇p = Y · ∂p.
B.2 Tensors living on q 2 = 0 in R 1,3 and projection onto the boundary On the two dimensional celestial sphere, any spin-J symmetric traceless tensor f a 1 ···a J (w,w) has only two independent components. In terms of complex coordinates w,w, we consider the components since all other components are forced to vanish due to the tracelessness condition. We can think of (B.8) as all plus or all minus spin components respectively, since they involve w orw indices exclusively. However, these components are not complex conjugates of each other in general.

JHEP06(2020)079
In our case of interest, we are dealing with f J (w,w) andf J (w,w) defined as pull-backs to the celestial sphere from a R 1,3 symmetric traceless tensor F µ 1 ···µ J (q) living on q 2 = 0, such that where F is transverse q µ i F µ 1 ···µ J (q) = 0. Thanks to (2.8) and the transversality condition, each Minkowski dimension of tensor F µ 1 ···µ J (q) can be expanded on the basis of vectors ∂ w q µ , ∂wq µ and q µ , with coefficients: However, note that in (B.9) only contractions with the terms ∂ w q µ or ∂wq µ appear, and q µ ∂ w q µ = q µ ∂wq µ = 0. This means that only two out of three vectors of the expansion on the second line in (B.10) contribute; or, equivalently, that the coefficient of q µ may be dropped. This tells us that while a tensor F of interest in general is not expected to be transverse with respect to v µ , eq. (B.9) remains unchanged if we project F to additionally be v µ -transverse v µ i F µ 1 ···µ J (q) = 0. 9 For convenience, we include this additional transversality in the following. The above properties are consistent with the fact that only two tensor components on the celestial sphere are non-zero, since the mixed-index projection vanishes automatically.
For example, f ww = ∂q µ ∂w ∂q ν ∂w F µν (q) = 2η µν − ∂q µ ∂w ∂q ν ∂w −2q µ v ν −2v µ q ν F µν (q) = −fw w = 0 (B.11) where we have used (2.8) in the second step, transversality and tracelessness in the third, and symmetry of f ab in the fourth (a quantity that is equal to plus or minus itself must be zero).

JHEP06(2020)079
Applying (B.19) repeatedly in the powers ((∂ w q) · R) J and ((∂wq) · R) J , we observe which means that all spin plus or all spin minus pull-back of a symmetric traceless transverse tensor F to the celestial sphere is equivalent to the same pull-back of the corresponding symmetric transverse (not-traceless) tensor F , which explains the simplification in (2.30).
For two spin-J symmetric traceless tensors f 1 and f 2 on C the tensor contraction is given by Using (2.8) and the fact that F 1 and F 2 are transverse and traceless, it is easy to see that this is equal to the contraction between their embedding space counterparts [31] f (B.23) Since both, F 1 and F 2 are transverse, all occurrences of q ν in the definition (B.14) of operator R µ vanish, so that R µ simplifies to an operator called D Z µ and the contraction effectively reads 1 J! d−2 2 J F 1 (q, R)F 2 (q, Z) = 1 J! d−2 2 J F 1 (q, D Z )F 2 (q, Z). (B.24) The simpler operator D Z µ is given by This explicitly demonstrates the connection with eqs. (3.29) and (3.30) in [31].
C Example spinning massive amplitudes mapped to the celestial sphere The simplest examples of amplitudes involving at least one massive spinning external particle are three-point amplitudes of a massive spinning particle of spin s and two massless scalars. In Minkowski space such three-point couplings are fixed to where the massive polarization tensor 1 µ 1 ...µs a for the first particle, e.g., in case of spin s = 1 or s = 2 is parametrized as in (A.1) or (A.3), and momenta p µ 1 = mp µ 1 and p µ 2 = ω 2 q µ 2 , p µ 3 = ω 3 q µ 3 as in (2.4) and (2.5).