Fuzzy de Sitter Space

We discuss properties of fuzzy de Sitter space defined by means of algebra of the de Sitter group $\mathrm{SO}(1,4)$ in unitary irreducible representations. It was shown before that this fuzzy space has local frames with metrics that reduce, in the commutative limit, to the de Sitter metric. Here we determine spectra of the embedding coordinates for $(\rho,s=\frac 12)$ unitary irreducible representations of the principal continuous series of the $\mathrm{SO}(1,4)$. The result is obtained in the Hilbert space representation, but using representation theory it can be generalized to all representations of the principal continuous series.


Introduction
Understanding of the structure of spacetime at very small scales is one of the most challenging problems in theoretical physics: more so as it is, as we commonly believe, related to the properties of gravity at small scales, that is to quantization of gravity. In the absence of a sufficient amount of experimental data, it is presently approached by mathematical methods: still there are basic tests which every model of quantum spacetime has to satisfy, as the mathematical consistency and the existence of a classical limit, usually to general relativity.
A feature very often discussed in relation to quantization is discreteness of spacetime.
Discreteness can mathematically be implemented in various ways, for example by endowing spacetime with lattice or simplicial structure. When discreteness is introduced by means of representation of the position vector by noncommuting operators or matrices we speak of fuzzy spaces. Assumption that coordinates are operators comes from quantum mechanics: fact it is in quite natural (perhaps even too elementary) to presume that generalization of [x µ , x ν ] = 0 to [x µ , x ν ] = 0 describes the shift of physical description to lower length scales. Operator representation has a potential to solve various problems of classical gravity and quantum field theory: it introduces minimal length, which in the dual, momentum space, can in principle resolve the problem of UV divergences; singular configurations of gravitational field can potentially be dismissed as corresponding to non-normalizable states, and so on. In addition, algebraic representation allows for a straightforward description of spacetime symmetries. Perhaps the main drawback of the assumption of discreteness is a loss of geometric intuition which is in many ways inbuilt in our understanding of gravity.
There are various ways to generalize geometry: one of the most important parts of any generalization is the definition of smoothness. In noncommutative geometry, derivatives are usually given by commutators; once they are defined, one can proceed more or less straightforwardly to differential geometry. We shall in the following use a variant of noncommutative differential geometry which was introduced by Madore, known as the noncommutative frame formalism, [1]. It is a noncommutative generalization of the Cartan moving frame formalism and gives a very natural way to describe gravity on curved noncommutative spacetimes. In particular classical, that is commutative, limit of such noncommutative 2 geometry is usually straightforward. Let us introduce the notation. Noncommutative space is an algebra A generated by coordinates x µ which are hermitian operators; fields are functions φ(x µ ) on A. Derivations or vector fields are represented by commutators. A special set of derivations e α can be chosen to define the moving frame, Derivations e α are generated by antihermitian operators, momenta p α , which can but need not belong to algebra A. 1-forms θ α dual to e α define the differential, Supplementary condition which allows to interpret θ α as a locally orthonormal basis is [φ, θ α ] = 0. In addition, one imposes consistency constraints on both structures, algebraic (associativity) and differential (d 2 = 0), and compatibility relations between them.
General features of the noncommutative frame formalism and many applications to gravity are known, [2]; the aim of our present investigation is to construct four-dimensional noncommutative spacetimes which correspond to known classical configurations of gravitational field. This means, to find algebras and differential structures which are noncommutative versions of, for example, black holes or cosmologies. One very important idea in this context is that spacetimes of high symmetry can be naturally represented within the algebras of the symmetry groups. The first model of such noncommutative geometry was the fuzzy sphere [3]: it has a number of remarkable properties which make it a role example for understanding what fuzzy geometry should or could mean. Different properties of the fuzzy sphere were used as guidelines to define other fuzzy spaces [4], including for us very important noncommutative de Sitter space in two and four dimensions [5,6,7]. In our previous paper [8] we analyzed differential-geometric properties of fuzzy de Sitter space in four dimensions realized within the algebra of the SO(1, 4) group. We found two different differential structures with the de Sitter metric as commutative limit. Here we analyze geometry of fuzzy de Sitter space that is the spectra of the embedding coordinates.
The plan of the paper is the following. In Section 2 we introduce notation for the SO(1, 4), review some results of [8] and discuss the flat limit of fuzzy de Sitter space revealing its 3 relation to the Snyder space. In Section 3 we solve the eigenvalueproblem of coordinates in the unitary irreducible representation (ρ, s = 1 2 ) of the principal continuous series. The obtaned spectrum we compare to the known group-theoretic result in Section 4.

Metric and scaling limits
We start with the algebra of the de Sitter group SO(1, 4) with generators M αβ , (α, β = 0, 1, 2, 3, 4) and signature 3) The only W -symbol of the SO(1, 4) group, [9], is the vector W α which is quadratic in the generators The Casimir operators of are It is obvious that there is a strong analogy between commutative four-dimensional de Sitter space described as an embedding in five flat dimensions, (2.8) and the Casimir relation It is therefore natural identify W α with the embedding coordinates, as first proposed in [5], and to define fuzzy de Sitter space as a unitary irreducible representation (UIR) of the so (1,4) algebra. This definition makes sense † in all cases except when W = 0, that is, for Class-I irreducible representations.
Group generators are dimensionless so a constant ℓ is introduced in (2.10) to give x α a dimension of length ‡ . There are two scales in our problem: the cosmological constant, Λ ∼ (10 26 m) −2 , and the Planck length, ℓ P l ∼ 10 −35 m. In preference to ℓ P l we will use third constant, noncommutativity parameterk, and assume that ℓ 2 P l <k < (10 −19 m) 2 . (2.11) The upper bound in (2.11) is a rough experimental limit tok. Assumption which is often taken,k ≈ ℓ 2 P l , would indicate that noncommutative geometry is directly related to quantization of gravity; a more moderate (2.11) means that noncommutative geometry is or might be an effective description of quantized gravity in the appropriate range of distances. We thus scale coordinates as Then the relation between the quartic Casimir operator and the cosmological constant (2.13) † That is, it has a straightforward meaning; see a comment related to double scaling limits given below. ‡ As we use units in which = 1, momenta have dimension of the inverse length.
Relations as (2.12) define the quantization condition. Dimensionally, we could have assumed a more general relation of the form but we chose the simplest, n = 0. For an interesting discussion of the quantization condition defined with respect to the Compton wavelength of the elementary system, see [6].
Limitk → 0 is the commutative limit of fuzzy de Sitter space. From we see that position commutator is proportional tok, that is, fork → 0 coordinates commute. The flat (noncommutative) limit on the other hand can be obtained when we consider de Sitter space in a 'small neighbourhood' of a specific point, for example at the north pole, for Λ → 0. At the level of the symmetry group this limit is defined by the Inönü-Wigner contraction (2.7). Commutation relations contract to and it is consistent to take Denotingk/(2µ 2 ) = a 2 , we see that we obtained the dual to the Snyder algebra. Namely, we found whereas the position algebra of [10] reads The limit µ → ∞ corresponds to a → 0.
In [8], two sets of momenta that define fuzzy geometries with correct commutative limits to classical de Sitter space were proposed. In the noncommutative frame formalism, fulfil stricter requirements than coordinates: first, they close into an algebra which is at most quadratic. In addition, if we wish to interpret tetrad e α A and metric g αβ = η AB e α A e β B as fields, we have to require that the frame elements depend only on coordinates, It is simplest to choose p A among the group generators § . When momenta close into a Lie algebra, [p A , p B ] = C D AB p D , the curvature defined in the framework of the noncommutative frame formalism is constant [1], and the curvature scalar is given by This means in particular that, in our case, momenta scale as √ Λ .
The second choice of momenta is (2.26) § See, however, comments given in the Appendix.
There are now four frame 1-formsθ α , α = 0, 1, 2, 3. Calculating the spacetime components of the metric, for (the noncommutative equivalent of) the line element we find This noncommutative metric and the corresponding moving frame do not possess the complete de Sitter symmetry. Normalization of the scalar curvature to the usual value gives ζ = 16/3.

Coordinates
Let us consider the spectra of the embedding coordinates x α . Classification of the unitary irreducible representations of the de Sitter group was done in [11,12,13]; the UIR's of the SO(1, 4) are induced from representations of its maximal compact subgroup SO(4).

8
In the discrete case there are two inequivalent representations π ± s,q for each value of q and s; values of the Casimir operators are discrete.
Using known matrix elements of M αβ from [13], one can calculate matrix elements of W α in basis {f k,k ′ m,m ′ }. We find Constants A k,k ′ , B k,k ′ , C k,k ′ , D k,k ′ are given for each concrete representation in [13]. From (3.29) we see that W 0 has discrete spectrum as noted in [5]. On the other hand, the eigenvalue equation for W 4 (and likewise for W i ) is quite difficult, if at all possible, to solve in this basis.
We therefore restrict to simpler problem: to find the eigenvalues of W α for a specific class of representations. The simplest possibility would be to consider Class I UIR's (they are in the principal and complementary series): their Hilbert space representations are known, they have a lowest weight state so the coherent states can be constructed, etc. However, Class I is characterized by condition W = 0: thus in our framework these UIR's cannot be simply interpreted as de Sitter spaces: a fixedk implies Λ → ∞ . Another subset which is singled out mathematically and physically is the principal continuous series. As shown in [14], in the Wigner-Inönü contraction limit these UIR's contract to a sum of two representations of the Poincaré group with positive value of the mass-squared. The Hilbert space representations of the principal continuos series were found in [15,16]: we shall perform the construction explicitly in the simplest nontrivial case, s = 1/2.
We start from the s = 0 representation of the principal continuous series. The representation space is a direct sum of the two s = 0 representation spaces of the Poincaré algebra, [15]. The states in each summand are wave functions in momentum space ψ( p), with the scalar product given by and

33)
It is on the other hand certainly possible to define specific double scaling limits, in order to interpret Class I representations as fuzzy de Sitter spaces; this point remains to be explored.
They are hermitian with respect to the given scalar product, and one can easily check that W α | s=0 = 0 , therefore W = 0 for (ρ, s = 0).
Higher spin representations (ρ, s) can be obtained from (ρ, s = 0) by adding spin generators S αβ to orbital generators L αβ . Representation space will be again a direct sum of two spaces, each equivalent to the Hilbert space of the Bargmann-Wigner representation of the Poincaré group of a fixed spin s, [17]. We shall here discuss the eigenvalue problem for s = 1 2 ; the case of higher spins is more involved because of an additional projection to the highest spin states, [19]. In addition, we will consider just a 'half' of the representation space, the other half being equivalent, [16].
States for s = 1 2 are Dirac bispinors in momentum space ψ( p) which are solutions to the Dirac equation. The Bargmann-Wigner scalar product is given by and the scalar product reduces to In the chiral representation which we will use later,γ 0 = 0 I I 0 ,γ i = 0 −σ i σ i 0 and the states can be parametrized as while the scalar product becomes The de Sitter group generators are given by hermiticity condition reads, in the Dirac representation of γ-matrices, From (3.33-3.36) we find the components W α : We have seen already in (3.29) that the spectrum of W 0 is discrete in every UIR of the SO(1, 4) group, and that the eigenvalues are k ′ (k ′ + 1) − k(k + 1) . On the other hand, due to de Sitter symmetry, spatial directions i and 4 are equivalent: therefore W 4 and W i have the same spectra. We can thus confine to the eigenvalue problem of W 4 .
We proceed as follows. First, we observe that in the Dirac representation W 4 has the form Unitary transformation to the chiral representation transforms W 4 tõ is automatically satisfied for A, B given by (3.51).
Since W 4 commutes with the generators of 3-rotations, we can diagonalize A + B simultaneously with M ij , that is, we can write the eigenfunctions in the form where p is the radial momentum, p 2 = (p i ) 2 = p 2 0 − m 2 and The Y m l are the spherical harmonics. The φ jm and χ jm are orthonormal and, [18] (3.56) Identity ( r · σ)( p · σ) = 3i + ip ∂ ∂p + i L · σ is also frequently used in the calculation.
Introducing Ansatz (3.55), we obtain the system Making the change of functions we get the first order system of equations The corresponding second order equations for F and H are and Two linearly independent solutions to the Legendre equation (5.80) are the associated Legendre functions P µ ν (x) and Q µ ν (x), or P µ ν (x) and P −µ ν (x). For (3.66-3.67), two linearly independent pairs of solutions arẽ so the normalization and the phases can be fixed as .

Group-theoretic view
In the previous section we solved the eigenvalueproblem of W 4 in (ρ, s = 1 2 ) UIR of the principal continuous series of SO (1,4) using the Hilbert space representation [15]. But This can be easily seen from their definition: where ǫ 0ijk4 = ǫ ijk . As W 0 is a Casimir operator of the compact group SO(4), it has discrete eigenvalues which are equal to k ′ (k ′ + 1) − k(k + 1). On the other hand, to find the eigenvalues of W 4 one has to decompose representation (ρ, s) or (ρ, s = 1 2 ) of the principal continuos series of SO (1,4) into the UIR's of its subgroup SO (1,3). This was done by  Our result for s = 1 2 is in accordance with this. There is only one summand in (4.75) corresponding to s 0 = s = 1 2 ; the spectrum of W 0 is the real axis, λ = ν 2 ∈ (−∞, +∞) . An analogous decomposition of unitary irreducible representations of the Poincaré group into a direct integral of UIR's of the Lorentz group was done in [21]: as we here use the same representation space [15], there are many paralells in two calculations. There are other operators, that is other coordinates on fuzzy de Sitter space whose properties one would like to understand and physically interpret. First of them is certainly the cosmological time, τ = −ℓ log (W 0 + W 4 ), and second are the isotropic coordinates. While it is, at least in the (ρ, s = 1 2 ) representation, straightforward to write the eigenvalueproblem for τ , the corresponding differential equation turns out to be not easy to solve. This is one of the problems in the given setup which deserves additional work and which might give interesting results.

Summary and outlook
The given construction of fuzzy de Sitter space can be straightforwardly generalized to other spaces of maximal symmetry with the symmetry groups SO(p, q), in particular for even-dimensional spaces, p + q = d + 1 with even d. In these cases, embedding coordinates can, as for d = 4, be identified with the highest W -symbol, is well studied, in particular, the decomposition formulas for the UIR's of the principal continuous series, [22] are known. Moreover, the algebra of the conformal group has the same structure that was used to define differential calculus for fuzzy de Sitter space in four dimensions. Clearly, for arbitrary dimension d momenta can be defined analogously to Thep i mutually commute; the differential structure which corresponds to this choice of the moving frame gives, in the commutative limit, metric of the de Siter space in d dimensions.
Therefore, a general construction with common general properties exists and should be further explored.
Acknowledgement Authors are very much indebted to the referee for pointing out a mistake in the calculation of the spectrum (which was present in the first version of the paper) as well as for relating the given derivation to the decomposition of the UIR's of SO (1,4) with respect to the UIR's of its subgroups. This work was supported by the Serbian Ministry of Education, Science and Technological Development Grant ON171031, and by the COST action MP 1405 "Quantum structure of spacetime".
This expression vanishes at the lower bound x = 1, while at the upper bound we use the asymptotics (5.84). We obtain .