Gravitational Waves in Locally Rotationally Symmetric (LRS) Class II Cosmologies

In this work we consider perturbations of homogeneous and hypersurface orthogonal cosmological backgrounds with local rotational symmetry (LRS), using a method based on the 1 + 1 + 2 covariant split of spacetime. The backgrounds, of LRS class II, are characterised by that the vorticity, the twist of the 2-sheets, and the magnetic part of the Weyl tensor all vanish. They include the flat Friedmann universe as a special case. The matter contents of the perturbed spacetimes are given by vorticity-free perfect fluids, but otherwise the perturbations are arbitrary and describe gravitational, shear, and density waves. All the perturbation variables can be given in terms of the time evolution of a set of six harmonic coefficients. This set decouples into one set of four coefficients with the density perturbations acting as source terms, and another set of two coefficients describing damped source-free gravitational waves with odd parity. We also consider the flat Friedmann universe, which~has been considered by several others using the 1 + 3 covariant split, as a check of the isotropic limit. In agreement with earlier results we find a second-order wavelike equation for the magnetic part of the Weyl tensor which decouples from the density gradient for the flat Friedmann universes. Assuming vanishing vector perturbations, including the density gradient, we find a similar equation for the electric part of the Weyl tensor, which was previously unnoticed.


I. INTRODUCTION
In light of the recent success in measurements of gravitational waves [1], and the consequent opening of a new observational window, it is of interest to study the propagation of gravitational waves and their interactions on different cosmological backgrounds to see, for example, what the effects of anisotropy and/or inhomogeneities are.
The fluctuations in the cosmic microwave background radiation (CMB), the large-scale structures and the cosmological redshift are well explained by the ΛCDM model [2][3][4][5][6], which describes an almost homogeneous and isotropic universe with a cosmological constant and cold dark matter. However, there are some deviations between the data and the model. For example, the observed power spectrum of the CMB seems to differs from the ΛCDM model for large angles [7][8][9][10]. Since a large amount of alternative matter is needed to account for the dark sector, a wide range of alternative cosmological models have also been investigated to explore if they can explain the current observations [11][12][13][14][15][16][17][18][19][20][21][22]. Also, present redshift studies do not give very strict bounds on the anisotropy in the expansion [23][24][25], making studies of different types of perturbations on anisotropic cosmological backgrounds of interest. For earlier works on this see, for example, [26][27][28][29][30][31], and for different perturbative methods see [32][33][34][35][36].
In this paper we will use a method based on the 1 + 3 and 1 + 1 + 2 covariant splits of spacetime [37][38][39][40][41][42][43][44][45][46][47][48] to study perturbations on anisotropic backgrounds. In the 1 + 3 split there is a preferred timelike vector, like the 4-velocity of matter, which is used to split tensors into timelike scalars and spacelike 3-tensors in a way that keeps covariance of the tensors. Similarly, a further 1 + 2 split can be made with respect to a spatial direction. This split is natural when there is a preferred spatial direction on the background, but can be also be used for isotropic backgrounds. Hence, the direction is fixed by, for example, choosing one of the perturbed vectors along it. The gauge problem in relativistic perturbation theory is here avoided by using covariant objects which vanish on the background for the perturbed quantities [49].
In an earlier paper [50] we considered perturbations on a Kantowski-Sachs background, using the 1 + 1 + 2 covariant split of spacetime [45]. The perturbations were vorticity-free and the perturbed spacetime was considered to be described by a perfect fluid. The perturbations include density fluctuations, shear waves, and pure gravitational perturbations travelling with the speed of light at leading order in the high frequency limit. Moreover, beyond this geometrical optics limit, anisotropic dispersion relations were indicated. The full dynamics were found to be given by evolution equations for six harmonic coefficients which decouple into two sub-systems, one with two components describing pure gravitational degrees of freedom, and one with the remaining four coefficients where the density gradient acts as a source term.
In this work we extend the previous 1 + 1 + 2 analysis to a wider class of locally rotationally symmetric (LRS) backgrounds. LRS symmetry means that spacetime is invariant under rotations around at least one spatial direction at every point [51,52]. The analysis will cover vorticity-free perturbations of all LRS spatially homogeneous and hypersurface orthogonal perfect fluid backgrounds with vanishing magnetic part of the Weyl tensor, except the hyperbolic and closed Friedmann models, which together with the flat model have been considered by several authors (see, for example, [37,[53][54][55][56][57][58][59] ), using the 1 + 3 split. The considered metrics all belong to LRS class II in the classification of [51]. We find the vorticity-free perturbations of the homogeneous and hypersurface orthogonal LRS II backgrounds to behave in an analogous way to those in the previous study on Kantowski-Sachs backgrounds [50] and a similar harmonic decomposition can be used. Still, all harmonic coefficients can be expressed in terms of six coefficients and the evolution equations have the same structure as before, but the behaviour of the solutions of course varies according to which backgrounds are taken. Finally, as a consistency check, we consider the flat Friedmann background as the isotropic limit of our 1 + 1 + 2 equations. We find that the magnetic part of the Weyl tensor, which in the general anisotropic case is partly sourced by the density gradient, satisfies a source-free second-order damped wave equation. This is in agreement with earlier results, using the 1 + 3 covariant split of spacetime. A second-order equation is also obtained for the electric part of the Weyl tensor for the case of pure tensor perturbations , in contrast to an earlier study [53].
The paper is organized as follows: In Section II a short summary of the 1 + 3 and 1 + 1 + 2 covariant splits of spacetime is given. The LRS backgrounds are discussed in Section III. In Section IV A the harmonic expansion is described and then the evolution equations for the harmonic coefficients are given in Section IV B. The high-frequency limit is considered in Section IV C. The flat Friedmann case is treated in Section IV D. Conclusions are summarised in Section V.

II. THE 1 + 3 AND 1 + 1 + 2 COVARIANT SPLITS OF SPACETIME
In this section we give a brief summary of the 1 + 3 and 1 + 1 + 2 covariant splits of spacetime. For more details on 1 + 3 split the reader is referred to [37,42] and for 1 + 1 + 2 split to [45,47]. A summary of the two can also be found in [50].
A 1+3 split of spacetime is suitable when there is a preferred timelike vector u a . The projection operator onto the perpendicular 3-space is given by h b a = g b a + u a u b in terms of the 4-metric g ab . With the help of h ab vectors and tensors can be covariantly decomposed into spatial and timelike parts. The covariant time derivative and projected spatial derivative are given byψ respectively. The covariant derivative of the 4-velocity, u a , can be decomposed as where the kinematic quantities of u a , acceleration, expansion, vorticity, and shear are defined by , and σ ab ≡ D <a u b> , respectively. Here square brackets [ ] denote anti-symmetrisation, and angular brackets < > denote the symmetric and trace-free part of a tensor, i.e. ψ <ab> ≡ h c (a h d b) − 1 3 h ab h cd ψ cd . These quantities, together with the Ricci tensor (expressed via the Einstein equations by, for example, energy density µ and pressure p for a perfect fluid) and the electric, E ab ≡ C acbd u c u d , and magnetic, H ab ≡ 1 2 ε ade C de bc u c , parts of the Weyl tensor, are then used as independent variables. Here The Ricci identities for u a and the Bianchi identities then provide evolution equations in the u a direction and constraints (see for example [42]).
A formalism for a further split (1 + 2) with respect to a preferred spatial vector n a (with u a n a = 0) was developed in [45,47]. Projections perpendicular to n a are made with N b a = h b a − n a n b , and in an analogous way to above, spatial vectors and tensors may be decomposed into scalars along n a and perpendicular two-vectors and symmetric, trace-free two-tensors as A a = An a + A a , ω a = Ωn a + Ω a , and σ ab = Σ(n a n b − 1 2 N ab ) + 2Σ (a n b) + Σ ab . This occurs similarly for E ab and H ab in terms of E, E a , E ab and H, H a , H ab , respectively. Derivatives along and perpendicular to n a are respectively. Similarly to the decomposition of ∇ a u b , D a n b , andṅ a can be decomposed into further kinematic quantities of n a as D a n b = n a a b + 1 2 φN ab + ξǫ ab + ζ ab andṅ a = Au a + α a , where a a ≡n a , φ ≡ δ a n a , ξ ≡ 1 2 ε ab δ a n b , ζ ab ≡ δ {a n b} , A ≡ n a A a , and α a ≡ N b aṅ b . The two-dimensional volume element is given by ε ab ≡ ε abc n c and curly brackets { } denote the symmetric and trace-free part of 2-tensors. A bar on vector indices will denote projection onto the 2-sheets, e.g.,ψā ≡ N b aψb . The Ricci and Bianchi identities are then written as constraints and evolution and propagation equations in the u a and n a directions, respectively (see [45]). For the commutation relations between the differential operators˙, and δ a when acting on scalars, vectors and tensors, see Appendix A.

III. LOCALLY ROTATIONALLY SYMMETRIC SPACETIMES
A spacetime which at each point is invariant under rotations around at least one spatial direction is referred to as locally rotationally symmetric, or LRS for short. The corresponding locally maximally symmetric 2-sheets perpendicular to the isotropy axis are characterized by the 2D curvature scalar R = 2K/a 2 2 , where a 2 is the radius of curvature (or alternatively the scale factor) and K = ±1 or 0 for spheres, pseudo-spheres, or planes, respectively.
The perfect fluid LRS spacetimes can be divided into three classes, I, II and III [51,52]. The Class I metrics are stationary with nonzero vorticity and vanishing shear and expansion and hence are of limited interest as cosmological models. Class II is characterized by the fact that the magnetic Weyl tensor H ab , vorticity ω ab , and 2-sheet twisting ξ all vanish. In general, spacetimes in this class are both time-and space-dependent and it contains many physically interesting solutions like spherically-symmetric perfect fluids, the inhomogeneous Lemaitre-Tolman-Bondi cosmologies, the homogeneous Kantowski-Sachs and LRS Bianchi I and III cosmologies, and the flat and hyperbolic Friedmann models. The metrics in LRS class III are spatially homogeneous with a nonzero twist of the 2-sheets and have vanishing vorticity and acceleration, as well as vanishing expansion of the 2-sheets. The only models in this class with vanishing magnetic part of the Weyl tensor are the closed Friedmann models.
Perturbations of Kantowski-Sachs universes, which are the hypersurface orthogonal and homogeneous LRS II models with positive 2-curvature, R > 0, were studied by us in an earlier paper [50]. In this paper we extend the analysis to all hypersurface orthogonal and homogeneous LRS II models with vanishing expansion of the 2-sheets, i.e., φ = 0. With this last requirement a similar harmonic decomposition as in [50] can be used. Fortunately this only excludes the hyperbolic Friedmann universes. Since the only solutions in LRS class III with vanishing magnetic part of the Weyl tensor are the closed Friedmann universes [60], it means that our analysis will cover all homogeneous and hypersurface orthogonal LRS backgrounds with a vanishing magnetic part of the Weyl tensor except the hyperbolic and closed Friedmann models, which together with the flat model have been studied elsewhere with the 1 + 3 covariant split (see e.g., [37,[53][54][55][57][58][59]).

A. LRS Class II
The perfect fluid LRS Class II spacetimes are characterised by H ab = ξ = ω ab = 0, see, e.g., [51,52]. In terms of the quantities defined in Section II, the spacetimes are given by the following scalars: the energy density µ, the pressure p, the electric part of the Weyl tensor E, the expansion Θ, the shear Σ, the acceleration A, and the expansion of the 2-sheets, φ. Alternatively, one of the quantities can be replaced with the 2-curvature of the 2-sheets For a complete local description of the geometry, the frame vectors along the 4-velocity, u a , and the preferred spatial direction, n a , are needed to construct all Cartan invariants (see e.g., [61]). In terms of timelike and spacelike coordinates, t and z, respectively, they are given by where X, x, Y and y are functions of t and z. For spatially homogeneous spacetimes, where all invariant objects are functions of a timelike coordinate solely, we may without loss of generality change the time coordinate so that X = 1 and x = 0. Metrics with 4-velocity u a orthogonal to the hypersurfaces of homogeneity are obtained by putting Y = 0.
The assumption of Y = 0 implies that R = 0 (see [52]), and give rise to tilted models of Bianchi types V or I. The quantities {µ, p, E, Θ, Σ, A, φ, X, Y, x, y}, which describe the spacetime, are subject to integrability conditions given by commutator equations between e 0 and e 1 , the Ricci equations for u a and n a , and some of the Bianchi identities (see [52,61,62]). Einstein's equations are imposed through the Ricci tensor, which for a perfect fluid is given by µ, p and u a .

Homogeneous and Hypersurface Orthogonal LRS II Metrics
With the assumptions x = Y = 0, it follows that the acceleration vanishes, A = 0, [52]. The system then reduces to the following evolution equations:μ where a dot indicates derivative with respect to t, and to the constraints

Homogeneous and Hypersurface Orthogonal LRS II Metrics with φ = 0
For φ = 0 the system reduces toμ with E given algebraically by Hence, given an equation of state p = p (µ) the solutions are completely determined in terms of Σ, Θ and µ, and the nonzero zeroth order quantities are given by the set S (0) = {Σ, Θ, µ, p, E}.
The 2-curvature is now given by where in the last equality the scale factor of the 2-sheets a 2 = a 2 (t) has been introduced and where K takes the values ±1 or 0 according to the geometry of the 2-sheets: sphere, pseudo-sphere, or flat. Taking the time derivative of R, and using Equations (14)- (16), one findsṘ and hence one of the evolution Equations (14)- (16) can be replaced by Equation (19). According to the sign of R, different types of solutions are obtained. For R > 0 one gets the Kantowski-Sachs cosmologies, which we studied in [50]. If R < 0 the spacetimes are of Bianchi type III. For R = 0 there are solutions of Bianchi type I/VII 0 , including the flat Friedmann universe. Since Equation (18) determines one of the quantities algebraically, one of the evolution equations can be dropped. This is due to the fact that the time derivative of Equation (18) will be identically satisfied due to the evolution Equations (14)- (16). The line-element can for the different values of K be written as where f 1 (ϑ) = sin 2 ϑ, f −1 (ϑ) = sinh 2 ϑ, and f 0 (ϑ) = 1 (or alternatively f 0 = ϑ). For K = 1 the 2-sheets are spheres and ϑ and ϕ the usual spherical coordinates, but for K = −1 and 0 the 2-sheets can be taken to be open and infinite with the topology of R 2 . The coordinates are dimensionless and hence the scale factors carry the dimension of length (or time since c = 1). The 4-velocity of comoving observers is u = ∂/∂t and the direction of anisotropy is n = a −1 1 ∂/∂z, which due to symmetry and normalisation satisfies [51]: In terms of of the scale factors a 1 and a 2 in (20), the expansion and scalar part of the shear take the values 3. Homogeneous and Hypersurface Orthogonal LRS II Metrics with φ = 0 There are also solutions with R = 0 and Σ = E = 0. For these the sheet expansion φ is in general nonzero and the system is given by Equations (14) and (15) plus the constraint If φ = 0, these are the negatively curved Friedmann models of Bianchi type V, whereas φ = 0 gives the flat Friedmann models which are covered by the sub-class in Section III A 2. For the negatively curved Friedmann models the metric can be given by

IV. VORTICITY-FREE, PERFECT FLUID PERTURBATIONS OF HOMOGENEOUS AND ORTHOGONAL LRS II COSMOLOGIES
The analysis of perturbations on Kantowski-Sachs backgrounds in [50] will here be extended to all homogeneous and hypersurface orthogonal LRS class II backgrounds except for the hyperbolic Friedmann models. As for Kantowski-Sachs we will assume that the perturbations are irrotational, i.e., that Ω = Ω a = 0, and also that the perturbed spacetime is described by a perfect fluid. The frame is partly fixed by choosing the preferred timelike vector u a to be the 4-velocity of the fluid also in the perturbed spacetime. Since the preferred direction n a is not kept for the perturbed spacetime, we choose to fix its direction by choosing a a = 0, meaning that the acceleration only has a component in the n a -direction. For more details on the fixing of frame, see [50].
The choice of frame does not completely fix the mapping between the perturbed and background spacetimes [37], but according to the Stewart-Walker lemma [49] variables which vanish on the background are gauge-invariant. Hence, for the generic case with φ = 0 on the background, we will replace the nonzero quantities on the background, µ, p, Θ, Σ and E with their gradients As was shown in [50] the hat derivatives, Θ etc., are determined in terms of the 2-gradients, W a etc., when the vorticity vanishes (see also Section IV A 2). The first-order variables which vanish on the background are then These are now subject to the Ricci identities for u a and n a and Bianchi identities, giving evolution equations along u a , propagation equations along n a and constraints. The exact, non-perturbative system of equations for a 1 + 1 + 2 split of spacetime can be found in [45]. For first-order perturbations the set of equations in terms of the new variables in Equation (26) was derived in [50]. This was done for Kantowski-Sachs backgrounds, but this set is actually valid for all hypersurface orthogonal homogeneous LRS class II spacetimes with φ = 0, the differences lying in the zeroth order coefficients for different backgrounds. For completeness we quote the result from [50] in Appendix B.
For the special case R = E = Σ = 0 and φ = 0 we should in a similar way use the variable φ a = δ a φ, whereas E and Σ now are of first order. For the modified system see Appendix C.

A. Harmonic Expansion
For the metrics given by Equation (20), where φ = 0, the wave equation on scalars is separable by applying the following harmonic expansion where the coefficients Ψ S k k ⊥ depend solely on time (see, e.g., [45,50,63]). The function P k is the eigenfunction of the Laplacian ∆ = n a ∇ a n b ∇ b and it is constant on the z = const hypersurfaces Here, k are the dimensionless constant comoving wave numbers in the direction of anisotropy, and a 1 is the scale factor in this direction. The physical wave numbers are given by k /a 1 .
Similarly, harmonics Q k ⊥ are introduced on the 2-sheets as eigenfunctions to the two-dimensional Laplace-Beltrami operator [45]: Here, δ 2 = δ a δ a , a 2 is the scale factor of the 2-sheets, and k ⊥ are the dimensionless comoving wavenumbers along the 2-sheets.
When R > 0 the 2-sheets are spheres and the harmonics can be represented by the usual spherical harmonics Y m with k 2 ⊥ = l(l + 1). Here l = 0, 1, 2, ..., and for a given l value the index m runs from −l to l. The index m does not occur in the equations governing the perturbations due to the background spacetime symmetries.
For R ≤ 0, when the 2-sheets are open, the k ⊥ are not discrete and may take any real values. For R = 0 the eigenfunctions can be represented by plane waves.
Vectors and tensors can be also expanded in harmonics by introducing vector and tensor harmonics [47,64,65]. The even (electric) and odd (magnetic) parity vector harmonics are and the vector Ψ a can be expanded as when the comoving wavenumbers take continous values, the sums are changed to integrals with a convenient normalization factor. For Q k ⊥ a and Q hold, respectively. This corresponds to the fact that a generic vector can be written as the sum of one curl-free and one divergence-free vector. Similarly, the even and odd tensor harmonics are and the tensor Ψ ab can be expanded as Note that for vectors Ψ a and tensors Ψ ab which are odd by definition, the rôles of quantities without and with an overbar, e.g., Ψ a , are interchanged. For example, for the magnetic part of the Weyl tensor, where the threedimensional volume element occurs in its definition, H T k k ⊥ belongs to the odd sector, whereas H T k k ⊥ belongs to the even sector.
Some useful relations involving the vector and tensor harmonics are listed in Appendix D. For different types of harmonics used in relativity and cosmology see, for example, [56,[66][67][68]].

Harmonics When φ = 0
In Bianchi V models with metric where z was introduced as z = ez, the source free wave equation for a scalar is: with In order to separate the time and spatial dependence of Ψ, we expand it in harmonics obeying where k is a real number. These harmonics can be built as follow. Equation (31) is modified to where k ⊥ is real and Q k ⊥ can be represented by plane waves: The expansion of Q k in harmonics Q k ⊥ is given by where the sum stands for a conveniently normalized integration with respect to k ⊥ and P k,k ⊥ (z) satisfies This equation was derived from (41) and (42) and by using φ = −2/a [45]. The regular solution of (45) is where K ν is the modified Bessel functions of the second kind with A scalar occurring at the first order in the perturbed spacetime can be expanded as Nevertheless, this expansion shows that a 1 + 3 covariant approach is more convenient in this case than the 1 + 1 + 2. The function P k,k ⊥ (z) depend on both separation constants k, k ⊥ . This is because δ 2 -derivative carries a z 2 factor in Equation (42).

Relations between Harmonic Coefficients
As was shown in [50], on using the commutation relation (A4) and the property (D6) of the vector harmonics and assuming vanishing vorticity, it follows that odd parts of the gradients of the scalars S (0) = {Σ, Θ, µ, p, E} defined in Equation (26) vanish: It was also shown that the harmonic coefficients of the hat derivatives of the objects in S (0) can be expressed in terms of the coefficients of the vectors in Equation (26). Denoting an object in S (0) by G its hat derivative can be expanded as and its 2-gradients G a ≡ δ a G as From (A3) it then follows that if Ω a and φ vanish to the zeroth order. where The system takes the same form as for the Kantowski-Sachs background [50], but note that the functions B, C etc. are slightly differently defined in terms of the curvature R of the 2-sheets and also that the solutions from Equations (14)-(16), (22) and (23) for the scale factors and kinematic quantities will be different for different values of R, given by Equation (18).
The system can also be written as two decoupled second-order wave equations with damping as where In the high-frequency limit the speed of propagation for these waves will approach the speed of light and hence they can be interpreted as free gravitational waves (see Section IV C).

System for
Here we have introduced the additional notations

C. High-Frequency Approximation
In [50], where the backgrounds were given by Kantowski-Sachs models, we studied the high-frequency limit (optical limit; see [71,72]), of the propagation equations. For our quantities this implies Since in this limit the curvature of the 2-sheets becomes negligible the resulting equations are identical in form to those for the Kantowski-Sachs backgrounds for all signs of R, but the zeroth-order factors a 1 , a 2 , Θ and Σ of course are different for different backgrounds.
For the uncoupled system of E T k k ⊥ and H T k k ⊥ the following second-order wave equations with damping where are obtained. These are in the formẌ where Ω is the undamped angular frequency and the actual angular frequency is given by Ω 1 − ζ 2 . The propagation speed of the wave is The propagation velocity hence goes as 1 − ζ 2 /2 for relatively small damping coefficients ζ, and approaches the speed of light for large frequencies. For the static case, when Θ = Σ = 0, the damping would vanish and then the propagation velocity would be exactly the speed of light. When the propagation is along the preferred direction, k ⊥ = 0, and q E 1 = q H1 , resulting in the same damping ζ || for both variables E T k k ⊥ and H T k k ⊥ . Hence, they have the same propagation velocity which differs from the speed of light at the second-order in ζ || . However, when the propagation is perpendicular to the preferred direction, k 2 = 0, then q E1 = q H1 , giving different dampings ζ ⊥E and ζ ⊥H for E T k k ⊥ and H T k k ⊥ , respectively. Therefore, the propagation velocities also differ at the second order in damping coefficients. In addition, since ζ || = ζ ⊥E = ζ ⊥H , the propagation velocities are direction-dependent.
As mentioned in Section IV B 2, the second-order equations for E T k k ⊥ and H T k k ⊥ also decouple from the density gradient in the high frequency limit and are given bÿ with q E1 = q H1 and q H1 = q E 1 . Beause of the latter, the propagation velocities of E T k k ⊥ and H T k k ⊥ and of H T k k ⊥ and E T k k ⊥ coincide in the high-frequency limit and as before the propagation velocity differs from the speed of light to the second order in the damping parameter.

D. Perturbations of the flat Friedmann models
Here we consider the flat Friedmann models as a check of the isotropic limit of the general LRS II case. In this case there is no preferred spatial direction on the background, but as before, we fix the 1-direction by choosing the acceleration to only have a 1-component, i.e., a a = 0, in the perturbed spacetime. Tensor perturbations of the Friedmann cases, using the 1 + 3 covariant split, were studied in [53] and we make a comparison with their results.
The flat Friedmann models are given by E = Σ = R = φ = 0. Without loss of generality we can use a 1 = a 2 ≡ a. We also introduce the notations and The first system for E T k k ⊥ and H T k k ⊥ then reduces tȯ As before, this can be written as second-order damped wave equations The term N is given by and vanishes in the high frequency limit.
The second system becomeṡ From these we obtain the following second-order wave equations for Σ T k k ⊥ and E T k k ⊥ , again with the density fluctuations acting as source terms, where The density gradient obeys the following second-order equation and we see that the density perturbations propagate with the speed of sound in the high frequency limit. Unlike the case with an anisotropic background, we now obtain a second-order decoupled wave equation for H Note that Equations (86) and (96) for H T k k ⊥ and H T k k ⊥ , respectively, are identical. Similarly, the left-hand sides of Equations (85) for E T k k ⊥ and (93) for E T k k ⊥ , respectively, are identical. The damping coefficients in the second-order equations depend only on k, therefore the propagation velocities of the perturbations are not direction-dependent. In addition the propagation velocities at high frequencies approach the speed of light. Because of the symmetries of Friedmann spacetimes, we can safely assume that µ V k k ⊥ depend only on k, and not separately on k and k ⊥ , which is also clear from Equation (95). Then the second-order equations for Σ T k k ⊥ and E T k k ⊥ also depend only on k like those governing E T k k ⊥ , H T k k ⊥ and H T k k ⊥ . In [53] the 1 + 3 covariant split was used to study tensorial perturbations of the Friedmann models. The pure tensor perturbations are characterised by vanishing energy density gradients and vorticity to the first order. Hence, when comparing our result with their we must use µ V k k ⊥ =μ V k k ⊥ = 0. Our Equations (86) and (96) for the even and odd parts of the magnetic part of the Weyl tensor, H T k k ⊥ and H T k k ⊥ , respectively, are then the same as their Equation (20) for the flat Friedmann case. The equation for Σ T k k ⊥ (92) similarly corresponds to their Equation (22) 1 .
The main difference between [53] and our result is that we obtain a second-order wave equation from Equation (93) for E T k k ⊥ , whereas they needed a third-order equation to decouple E ab . In Equation (15) in [53] they give a second-order equation for the electric part of the Weyl tensor, E ab , with the shear σ ab acting as a source term. From our Equation (88) we see that imposing µ V k k ⊥ =μ V k k ⊥ = 0 gives a constraint between Σ T k k ⊥ and H This constraint is satisfied as is seen by differentiating it and substituting Equations (89)-(91). Hence, the number of independent variables in the system (88)-(91) is reduced from four to two by imposing that the density perturbations vanish. With the help of Equation (90) now Σ T k k ⊥ can be completely expressed in terms of By using this result in their Equation (15) in for the flat Friedmann case, where simple plane waves can be used for the harmonics, we obtain our Equation (93). The three-dimensional Equations (7) and (21) in [53] correspond to our Equations (97) and (98). Using the three-dimensional harmonics in [68] similar second-order equations for all values of K are obtained (see Appendix F).

V. CONCLUSIONS
A previous analysis of vorticity-free perturbations on Kantowski-Sachs backgrounds has been extended to all homogeneous and hypersurface orthogonal LRS perfect fluids with the vanishing magnetic part of the Weyl tensor except the hyperbolic and closed Friedmann models, which have been studied elsewere [37,[53][54][55][57][58][59] using the covariant 1 + 3 split approach. We find the same structure of the evolution equations for the perturbations as in the case of Kantowski-Sachs. All harmonic coefficients can be determined in terms of a subset containing only six coefficients. The evolution equations for these decouple into one system for E T k k ⊥ and H T k k ⊥ , representing source-free gravitational degrees of freedom, and another for Σ T k k ⊥ , E T k k ⊥ , H T k k ⊥ , and µ V k k ⊥ , which describes perturbations sourced by the density gradient. Only in the high frequency limit do the second-order wave equations for E T k k ⊥ and H T k k ⊥ decouple from the source terms. The analysis of propagation velocities in the high frequency limit led to direction-dependent dispersion relations on anisotropic backgrounds.
We also studied perturbations on the flat Friedmann universe, which is the isotropic limit of the considered class of backgrounds. Here the second-order wave equation for H T k k ⊥ decouples from the other coefficients, whereas E T k k ⊥ still is sourced by the density gradient. The result is compared with an earlier study, [53], where a 1 + 3 formalism was used to study pure tensor perturbations on Friedmann backgrounds. The 1 + 1 + 2 covariant approach, together with a harmonic decomposition, is also effective for this setup, because all tensorial perturbations are easily obtained as second-order differential equations in contrast to the third-order equation more naturally appearing for the electric part of Weyl tensor in the 1 + 3 covariant description.

Acknowledgements
The work of ZK was partially supported by the UNKP-17-4 New National Excellence Program of the Ministry of Human Capacities and partially by the Hungarian National Research, Development and Innovation Office (NKFI) in the form of the grant 123996.

APPENDIX A: COMMUTATION RELATIONS
The commutation relations of covariant derivatives of the scalar field Ψ on hypersurface orthogonal and homogeneous LRS II backgrounds are to the first order: Similar relations hold for the first-order 2-vector Ψ a : and for the first-order symmetric, trace-free 2-tensor Ψ ab : where the 2-curvature R is given by Equation (18). In (A3) and (A7) the last terms on the right-hand sides are second-order in the generic case when φ = 0 on the background, and can hence be dropped.

APPENDIX B: EVOLUTION AND PROPAGATION EQUATIONS AND CONSTRAINTS FOR φ = 0
Here, the evolution and propagation equations and constraints from reference [50] for the generic case when φ = 0 are repeated. These are obtained by linearising the 1 + 1 + 2 equations in [45]. 2 The set S (0) = {Θ, Σ, E, µ, p} gives the quantities which are nonzero on the background. We define the corresponding first-order quantities which vanish on the background. The vorticity-free perturbations are then given by the following nonzero first-order quantities (which all vanish on the background): The evolution equations are given byφ Finally, the constraints are APPENDIX C: EVOLUTION AND PROPAGATION EQUATIONS AND CONSTRAINTS FOR φ = 0 Here, the evolution and propagation equations and constraints are given for the exceptional case where φ = 0 on the background, corresponding to the negatively curved Friedmann universe. The set S (0) = {Θ, µ, p, φ} gives the quantities which are nonzero on the background. We define corresponding first-order quantities which vanish on the background. As before, we let V a = δ a Σ and X a = δ a E. Vorticity-free perturbations hence are given by the following nonzero first-order quantities (which all vanish on the background): The following evolution equations then hold on the perturbed spacetimes: The equations containing both propagation and evolution contributions arė Eā The pure propagation equations are Finally, the constraints are

APPENDIX D: HARMONICS
In this Appendix we enlist a set of identities for the even Q k ⊥ a and odd Q k ⊥ a vector harmonics, including the orthogonality relations the algebraic relations and the differential relationsQ where the 2-curvature R is given by Equation (18). The even and odd tensor spherical harmonics obey the orthogonality relations the algebraic relations and the differential relationsQ

APPENDIX E: HARMONIC COEFFICIENTS
The perturbation variables coupled to µ V k k ⊥ , Σ T k k ⊥ , E T k k ⊥ , and H T k k ⊥ are