Cosmic microwave background CMB temperature and polarization observations indicate that in the bestfit Lambda Cold Dark Matter model of the Universe the local geometry is consistent with at most a small amount of positive or negative curvature i.e. vertOmegaKvertll1. However whether the geometry is flat E3 positively curved S3 or negatively curved H3 there are many possible topologies. Among the topologies of S3 geometry the lens spaces Lpq where p and q pgt1 and 0ltqltp are positive integers are quotients of the covering space of S3 the threesphere by mathbbZp the cyclic group of order p. We use the absence of any pair of circles on the CMB sky with matching patterns of temperature fluctuations to establish constraints on p and q as a function of the curvature scale that are considerably stronger than those previously asserted for most values of p and q. The smaller the value of vertOmegaKvert i.e. the larger the curvature radius the larger the maximum allowed value of p. For example if vertOmegaKvertsimeq 0.05 then pleq 9  while if vertOmegaKvertsimeq 0.02 p can be as high as 24. Future work will extend these constraints to a wider set of S3 topologies.
['Astrophysics - Cosmology and Nongalactic Astrophysics', 'General Relativity and Quantum Cosmology', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory']
Cosmic topology. Part Ic. Limits on lens spaces from circle searches
{'No Header': 'IFT-UAM/CSIC-24-118', 'Cosmic topology. Part Ic. Limits on lens spaces from circle searches': "(COMPACT Collaboration)  \n<!-- image -->  \nSamanta Saha, a Craig J. Copi, a Glenn D. Starkman, a Stefano Anselmi, b,c,d Javier Carrón Duque, e Mikel Martin Barandiaran, e Yashar Akrami, e,a,f Fernando Cornet-Gomez, a Andrew H. Jaffe, f Arthur Kosowsky, g Deyan P. Mihaylov, a Thiago S. Pereira, h Amirhossein Samandar, a and Andrius Tamosiunas a  \n- a CERCA/ISO, Department of Physics, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, Ohio 44106, USA\n- b INFN, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy\n- c Dipartimento di Fisica e Astronomia 'G. Galilei', Università degli Studi di Padova, via Marzolo 8, I-35131 Padova, Italy\n- d Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, Université Paris Cité, CNRS, F-92190 Meudon, France\n- e Instituto de Física Teórica (IFT) UA M-CSIC, C/ Nicolás Cabrera 13-15, Campus de Cantoblanco UAM, 28049 Madrid, Spain\n- f Astrophysics Group & Imperial Centre for Inference and Cosmology, Department of Physics, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, United Kingdom\n- g Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania 15260, USA\n- h Departamento de Física, Universidade Estadual de Londrina, Rod. Celso Garcia Cid, Km 380, 86057-970, Londrina, Paraná, Brazil  \nE-mail: samanta.saha@case.edu, craig.copi@case.edu, glenn.starkman@case.edu, stefano.anselmi@pd.infn.it, javier.carron@csic.es, mikel.martin@uam.es, yashar.akrami@csic.es, fernando.cornetgomez@case.edu, a.jaffe@imperial.ac.uk, kosowsky@pitt.edu, deyan.mihaylov@case.edu, tspereira@uel.br, amirhossein.samandar@case.edu, andrius.tamosiunas@case.edu  \nAbstract. Cosmic microwave background (CMB) temperature and polarization observations indicate that in the best-fit Λ Cold Dark Matter model of the Universe, the local geometry is consistent with at most a small amount of positive or negative curvature, i.e., | Ω K | /lessmuch 1. However, whether the geometry is flat ( E 3 ), positively curved ( S 3 ) or negatively curved ( H 3 ), there are many possible topologies. Among the topologies of S 3 geometry, the lens spaces L ( p, q ), where p and q ( p > 1 and 0 < q < p ) are positive integers, are quotients of the covering space of S 3 (the three-sphere) by Z p , the cyclic group of order p . We use the absence of any pair of circles on the CMB sky with matching patterns of temperature fluctuations to establish constraints on p and q as a function of the curvature scale that are considerably  \nstronger than those previously asserted for most values of p and q . The smaller the value of | Ω K | , i.e., the larger the curvature radius, the larger the maximum allowed value of p . For example, if | Ω K | /similarequal 0 . 05 then p ≤ 9, while if | Ω K | /similarequal 0 . 02, p can be as high as 24. Future work will extend these constraints to a wider set of S 3 topologies.  \nKeywords: cosmic topology, cosmic anomalies, statistical isotropy, cosmic microwave background, large-scale structure", '1 Introduction': "According to the general theory of relativity, the local geometry of spacetime is a solution of the Einstein field equations, a set of coupled, non-linear, local partial differential equations [1]. Assuming that appropriate spatial slices of that spacetime and its contents are homogeneous and isotropic, the local four-geometry will be described by one of the three Friedmann-Lemaître-Robertson-Walker (FLRW) metrics, i.e., one of the three isotropic, constant-curvature geometries-flat (zero spatial curvature) Euclidean geometry E 3 , positive spatial curvature S 3 , and negative spatial curvature H 3 -with a time-dependent scale factor.  \nThe metric, however, characterizes only the local geometry-one must independently specify the global structure of the spacetime. It is conventionally assumed that the spacetime manifold is time cross the covering space 1 of one of those three homogeneous, isotropic geometries-i.e., infinite flat 3-space (the covering space of E 3 ), the 3-sphere S 3 , or the 3-dimensional pseudosphere H 3 . However, while these covering spaces are the manifolds that globally preserve the isometry group of each local geometry, each homogeneous and isotropic 3-geometry admits many possible topologies, with at least one real parameter to specify the manifold with that topology.  \nThere are thus many possible 3-manifolds other than the three covering spaces that can accommodate FLRW cosmology. They are distinguished from the covering spaces in lacking globally the full isotropy 2 (and usually parity and homogeneity) of their local geometries. This global isotropy breaking, parity breaking, or homogeneity breaking has the potential to be reflected in the properties of fluctuations around the FLRW background, and thus in the statistical properties of cosmological observables. In recent work [2], we explored how symmetry breaking in non-trivial topologies affects cosmic microwave background (CMB) polarization correlation matrices.  \nIn this paper, we consider the possible spacetimes with S 3 spatial geometry, and place new limits on one class of allowed S 3 topologieslens spaces -as a function of the curvature scale. While 3-space on large scales is reasonably homogeneous and isotropic, there is evidence from CMB temperature fluctuations of multiple 'large-angle' anomalies. Together, these  \namount to evidence in excess of 5 σ equivalent significance against statistical isotropy [3], mostly on scales larger than the horizon size at the time of the last scattering of the CMB photons (see, e.g., Refs. [4-8] for reviews.) One of the very few potential physical explanations for this large-scale anisotropy is non-trivial spatial topology, though no specific manifold has yet been identified that explains the observed isotropy violation.  \nThe possibility of non-trivial spatial topology has been considered since at least as far back as Einstein's initial S 3 cosmological model [9] at which time de Sitter remarked [10] that the projective 3-sphere, which has the same local geometry but half the 3-volume, was to be preferred. Ever since, there have been cosmologists working to develop observational tests of cosmic topology. Several approaches have been considered, including cosmic crystallography (the search for topological 'clones') [11], CMB matched circle pairs (a.k.a. 'circles in the sky') [12-14] which is essentially the search for topological clones in CMB maps, and CMB Bayesian likelihood comparison [15-17]. More recently, the general set of eigenmodes, the correlation matrices, and the detectability of the orientable Euclidean manifolds have been studied in Refs. [2, 18-20]. Similarly, various machine learning techniques have been explored as tools for detecting signatures of non-trivial topology in harmonic space [21].  \nWhile, in principle, Bayesian likelihood comparison is the most powerful technique because it uses all the available data, it suffers the disadvantage that the likelihood must be computed for each allowed topology of each allowed 3-geometry, for every value of the real parameters that specify the 3-manifolds of a given topology, and for every distinguishable position and orientation of the observer within the manifold [15]. Moreover, that scan over the space of possible 3-manifolds should, at least in principle, be done at the same time as the scan over the space of parameters that specify the background cosmology. With a countable infinity of possible topologies, up to six additional parameters that specify the manifold (e.g., the lengths of the sides of a torus in E 3 ) and up to six parameters specifying the position and orientation of the observer within a manifold that breaks isotropy and homogeneity, in addition to the seven cosmological parameters, it is no surprise that the full Bayesian likelihood search has yet to be attempted. On the other hand, a search using the circles-in-the-sky method is agnostic to the cosmological parameters, agnostic to the local 3-geometry-so long as anisotropies in the 3-geometry are sufficiently small-and agnostic to the values of the topological parameters within the domain of validity of the search.  \nIn a topologically non-trivial spatial 3-manifold, points in the covering space of the local geometry are identified if they are related by any element of some discrete group of spatial transformations (a discrete, freely acting, subgroup of the isometry group of the local geometry). We call any such pair of identified points in the covering space 'clones' (or sometimes 'topological clones'). It is important to realize that these clones have no independent existence, but they are often a convenient way to visualize or calculate the consequences of non-trivial topology.  \nThe circles signature rests on two fundamental observations. First, the CMB photons have all been traveling through the Universe since very nearly the same time, i.e., since recombination of the primordial plasma, and therefore the CMB that any observer detects comes from a sphere centered on them-their last-scattering surface (LSS). Second, for every one of our clones that is closer to us than the diameter d LSS of the LSS, our LSS intersects with 'their' LSS and the intersection of those two spheres is a circle. This circle is a locus of points visible to us (i.e., to ourselves and our clone) in two distinct directions on the sky. 3 So  \nlong as that circle is large enough, we would be able to identify the tight correlation of CMB temperature fluctuations around the two matched circles as statistically anomalous, and so detect non-trivial topology.  \nThis search for matched-circle pairs was performed in full generality on the Wilkinson Microwave Anisotropy Probe (WMAP) full-sky temperature map and no statistically significant matches were found [14, 22, 23]. The search was repeated on Planck 2013 maps with identical results [24], but not reported. A limited search was conducted by the Planck team, again with negative outcome [16, 17]. In all cases, the smallest circle that could be ruled out depended on the required false negative and positive rates. However, both are steep functions of the radius of the circle for small circle size. 4  \nThe negative conclusion of these searches is that the length of the shortest path from us to our nearest clone, i.e., the shortest path around the Universe through us , must be greater than f O d LSS . The reported value of f O is 0 . 985 at 95% confidence level. The task remains to translate this generic limit on the distance to our nearest clone into a constraint on model parameters. In Ref. [19], this was done for orientable manifolds admitting homogeneous Euclidean geometry E 3 ; this will be complemented in a future paper on non-orientable E 3 manifolds. Here, we begin the same task for manifolds admitting a homogeneous S 3 local geometry by considering the lens spaces L ( p, q ): the quotient spaces of the spherical manifolds by the cyclic group Z p . A future paper will consider the other S 3 manifolds, and still other papers will in turn consider the six other Thurston geometries [25] as each presents its own particular challenges.  \nThis work is by no means the first attempt to constrain topologies of S 3 . A detailed construction and complete classification of all 3-dimensional spherical manifolds was given by Gausmann et al. [26]. They also discussed the likelihood of detectability of spherical topologies by crystallographic methods, as a function of cosmological parameters. Gomero et al. [27] considered which hyperbolic and spherical manifolds were excluded by observations, however, this was before the considerable progress made using WMAP data and then Planck data, and in particular they could not include constraints from matched-circle searches [14, 16, 17, 22, 23]. In the same period, Uzan et al. [28] studied CMB anisotropies in S 3 manifolds, focusing on the lens spaces L ( p, 1). Suppression of low/lscript anisotropies in inhomogeneous lens spaces L ( p, q ), especially with p = 8, was studied by Aurich et al. [29], followed by exploration of the specific L ( p, q = p/ 2 -1) with p (mod 4) = 0 and prism spaces [30]. In Ref. [31], the authors surveyed lens spaces with p ≤ 72 and concluded that L ( p, q ) with q ≈ 0 . 28 p and q ≈ 0 . 38 p display strong suppression of CMB fluctuations on angular scales θ ≥ 60 · compared with the covering space.  \nIt is important to note that, for all p and all allowed values of q (mod p ) > 1, L ( p, q ) is statistically inhomogeneous, i.e., the statistical properties of CMB anisotropies (and other observables) depend on the CMB observer's position. This is because translation invariance is broken by the requisite boundary conditions-for example, the length of the shortest closed geodesic varies with location. The q = 1 lens spaces are the rare exception. This means that any exploration of constraints on lens spaces must vary not only p , q , and the Ricci scalar, but also the location of the observer. Similarly both isotropy and parity are violated statistically; and so the orientation of the observer and the handedness of their coordinate system matter. In this paper, we systematically explore constraints on L ( p, q ), based on the fact that  \nmatched-circle pairs in the CMB temperature sky have not been detected. This, and a new analysis of clone separations in L ( p, q ), will allow us to considerably strengthen the previous limits on these spaces obtained in Ref. [27].  \nThis paper is organized as follows. We provide a brief review of the S 3 geometry and lens spaces L ( p, q ) in Section 2. The background for the application of circle searches to lens spaces is given in Section 3. To connect the circle searches to observational constraints requires understanding of S 3 cosmological models, which is presented in Section 4. In Section 5, we relate the non-detection of CMB matched-circle pairs to constraints on the parameters of the lens spaces and gives a strong condition on the detectability of the lens spaces as possible topologies of the Universe. We summarize the paper and conclude in Section 6.  \nThe GitHub repository associated with this study is publicly available at https://github. com/CompactCollaboration . Codes will be deposited there as publicly usable versions become available.", '2 3-sphere and lens spaces': "We begin with a short introduction to S 3 and, in particular, the lens spaces. Some details not pertinent to limits from circle searches are included to provide a more complete introduction and a foundation for future studies.  \nThere are various ways to discuss the 3-sphere, S 3 . We will describe it in terms of its natural embedding in 4-dimensional Euclidean space E 4 as the set of points { ( x 0 , x 1 , x 2 , x 3 ) | x 2 0 + x 2 1 + x 2 2 + x 2 3 = R 2 c } . For simplicity we will typically work in units of the curvature scale, i.e., we set R c = 1.  \nThe 3-sphere S 3 is both this simply-connected space (i.e., any closed loop on this 3-sphere can be smoothly contracted to a point) and the geometry induced on this 3-sphere. In this representation, it is manifest that the isometry group of S 3 is O (4)-the rotations and reflections in four dimensions. The topologically non-trivial manifolds with S 3 geometry are quotients of the 3-sphere by any freely acting discrete subgroup of the full isometry group. 5 For S 3 the freely acting discrete subgroups consist of only rotations, i.e., they are all discrete subgroups of SO (4), none of the freely acting isometries are parity-reversing. More simply put, one covers the 3-sphere with a finite number of identical tiles that are related to one another by (a finite set of) SO (4) elements, such that no point on the edge of one tile touches the identical point on a neighboring tile, and the tiles share only edges. There are a countably infinite number of such discrete subgroups of SO (4). Threlfall and Seifert [32] gave the first complete classification of these spherical 3-manifolds. Another classification method, using quaternions, can be found in Ref. [25]. In the cosmological context, a detailed and complete classification of all the spherical manifolds can be found in Ref. [26].  \nIn this paper, we focus on lens spaces, quotient spaces of S 3 of the form S 3 / Z p , where Z p is the cyclic group of order p (considered as a subgroup of SO (4)). There are multiple distinct actions of Z p on S 3 that give distinct spaces labeled by a second integer parameter q , where p and q are relatively prime and 0 < q < p [25]. The group of each of these actions has p elements, R j pq (with j ∈ { 0 , . . . , p -1 } ), acting on a point x ∈ S 3 by  \nx ' = ( R pq ) j x ≡ R j pq x . (2.1)  \nOne particularly useful representation of R j pq is as a rotation in E 4 separated into rotations in two orthogonal planes,  \nR j pq =      cos(2 πj/p ) -sin(2 πj/p ) 0 0 sin(2 πj/p ) cos(2 πj/p ) 0 0 0 0 cos(2 πjq/p ) -sin(2 πjq/p ) 0 0 sin(2 πjq/p ) cos(2 πjq/p )      . (2.2)  \nThis contains a rotation by (2 π/p ) j in the x 0 -x 1 plane simultaneously with a rotation in the x 2 -x 3 plane by (2 π/p )( jq (mod p )). Note that R j pq keeps both x 2 0 + x 2 1 and x 2 2 + x 2 3 unchanged-this will prove crucial for understanding the limit we will place on L ( p, q ).  \nClearly R p pq = R 0 pq ≡ 1 , while R pq ≡ R 1 pq is a generator of the group. 6 An object at a location x (0) would thus have p -1 distinct clones,  \nx ( j ) = R j pq x (0) , j ∈ { 1 , . . . , p -1 } . (2.3)  \nFor each choice of the value of p , it appears at first sight that there are up to p -1 distinct q values defining different lens spaces L ( p, q ) for q ∈ { 1 , . . . , p -1 } . Note that R p 0 is not freely acting, and that, if q > p , R pq = R p ( q (mod p )) , so we can indeed limit the analysis to 0 < q < p . In truth, not all of these values are allowed-some are not freely acting-and not all of them are distinct. However, let us first understand the role of q . To do so, consider the pattern of clones yielded by (2.3) given the representation of R pq in (2.2).  \nWe can label the clones of any point by the two integers j and j ' ≡ jq (mod p )-for a fixed p and q there will be p -1 clones of the initial point. Taking p = 7 as an example, for q = 1, the rotation R 71 takes ( j, j ' ) to (( j +1)(mod 7) , ( j ' +1)(mod 7)). Starting at ( j, j ' ) = (0 , 0), repeated applications of R 71 gives the ( j, j ' ) sequence  \n(0 , 0) → (1 , 1) → (2 , 2) → (3 , 3) → (4 , 4) → (5 , 5) → (6 , 6) → (0 , 0) . (2.4)  \nThis represents the 6 clones of a point labeled by (0 , 0) in L (7 , 1). Similarly, for q = 2, the rotation R 72 takes ( j, j ' ) → (( j +1)(mod 7) , ( j ' +2)(mod 7)), so starting at (0 , 0) repeated applications of R 72 takes  \n(0 , 0) → (1 , 2) → (2 , 4) → (3 , 6) → (4 , 1) → (5 , 3) → (6 , 5) → (0 , 0) . (2.5)  \nThis represents the 6 clones of a point labeled by (0 , 0) in L (7 , 2).  \nAn important question for cosmology is 'For a given value of p which values of q are physically distinct?' Roughly, two topological spaces S 1 and S 2 have 'similar shapes' if they are homeomorphic. More precisely, a function h : S 1 → S 2 is a homeomorphism if it is continuous, one-to-one and onto, and its inverse h -1 is also continuous. If such a function exists then the spaces S 1 and S 2 are homeomorphic. Two lens spaces L ( p, q ) and L ( p ' , q ' ) are known to be homeomorphic if and only if p = p ' and either q = ± q ' (mod p ) or qq ' = ± 1 (mod p ).  \nTopologically, L ( p, q ) and L ( p, q ' ) are equivalent if they are homeomorphic, resulting in catalogs of lens spaces only including one of each class. However, a homeomorphism does  \nnot preserve all physical properties. Thus, although spaces may 'have the same shape', they may still be physically distinguishable by observers in those spaces. As one example, L (7 , 2) and L (7 , 5) are homeomorphic since 2 = -5(mod 7). Notice that R 75 takes (0 , 0) to (1 , 5) which is equivalent to (1 , -2). Written in this more suggestive manner, if one starts at (0 , 0) repeated application of R 75 takes  \n(0 , 0) → (1 , -2) → (2 , -4) → (3 , -6) → (4 , -1) → (5 , -3) → (6 , -5) → (0 , 0) . (2.6)  \nComparing to (2.5) we see that these two spaces have opposite 'handedness,' in the sense that while j steps in the same direction for both spaces, j ' steps in opposite directions. Thus L (7 , 2) and L (7 , 5) have distinguishable clone patterns despite being homeomorphic. More generally, this is true for all L ( p, q ) and L ( p, p -q ): they are homeomorphic topological spaces but have distinguishable clone patterns. Note that for these pairs of topologies the distances between all pairs of clones will remain the same.  \nContinuing with p = 7, L (7 , 2) and L (7 , 3) are also homeomorphic since 2 × 3 = 6 = -1 (mod 7). Once again these spaces can be shown to have different clone patterns though the homeomorphism between the two spaces is less obvious. Despite this, the distance between all pairs of clones will also remain the same. Similarly, it can be shown that the pattern of clones seen by an observer in L (7 , 2) is identical to that seen by some observer in L (7 , 4) and the pattern of clones seen by an observer in L (7 , 3) is identical to that seen by some observer in L (7 , 5). 7 Wrapping up the example, this means that there are three physically distinct lens spaces for p = 7: L (7 , 1) and two additional ones that can be chosen to be L (7 , 2) and L (7 , 3). L (7 , 4), L (7 , 5) and L (7 , 6) are each physically equivalent to one of these three.  \nThe behavior of the p = 7 example is generic. L ( p, q ) is homeomorphic to L ( p, p -q ), but they do not share the same clone pattern. There is also at most one other 0 < q ' < /floorleft p/ 2 /floorright such that L ( p, q ' ) is homeomorphic to L ( p, q ) and with its clone pattern identical to that of L ( p, p -q ). The list of L ( p, q ) that are distinct for cosmological purposes is thus longer than the list of L ( p, q ) that are topologically distinct: for every topologically distinct L ( p, q ) with 0 < q < /floorleft p/ 2 /floorright , physically one must also consider L ( p, p -q ). If there is another homeomorphic L ( p, q ' ) with q ' < /floorleft p/ 2 /floorright , then it is physically equivalent to L ( p, p -q ). 8  \nWhile this holds in general, the focus of this work is on limits from circle searches which only depend on the interclone distances and not on the pattern of the clones. Therefore,  \n(0 , 0) → (1 , 4) → (2 , 1) → (3 , 5) → (4 , 2) → (5 , 6) → (6 , 3) → (0 , 0) .  \nWe see that these contain all the same clones (tuples of j and j ' ) if we swap j and j ' , i.e., if we swap ( x 0 , x 1 ) and ( x 2 , x 3 ). (The order in the sequence is irrelevant.) This swapping can be accomplished by the orthogonal transformation  \nO = ( 0 2 × 2 1 2 × 2 1 2 × 2 0 2 × 2 ) .  \nTherefore, L (7 , 2) and L (7 , 4) have the same clone patterns.  \n8 Topologists are also interested in spaces that are homotopically equivalent, a weaker condition than homeomorphic: all lens spaces that are homeomorphic are also homotopically equivalent, but the converse is not true. The two lens spaces L ( p, q ) and L ( p ' , q ' ) are homotopically equivalent if and only if p = p ' and qq ' = ± n 2 (mod p ) for some n ∈ Z . For example, L (11 , 2) and L (11 , 3) are homotopically equivalent since 2 × 3 = 6 = -4 2 (mod 11), but they are not homeomorphic. Note that p = 11 is the smallest p with both q and q ' larger than 1 for which there is a homotopically equivalent but not homeomorphic pair of lens spaces. Homotopically equivalent lens spaces that are not homeomorphic are physically distinguishable with different clone pair separations.  \nin this work we can restrict ourselves to 0 < q < /floorleft p/ 2 /floorright since the homeomorphic partners L ( p, p -q ) of each lens space have the same interclone distances.", '3 Circle search for lens spaces': "Constraints on the non-trivial topology of the Universe can be addressed by the existing circle-in-the-sky signature searches based on CMB temperature data. As noted above, for the lens space L ( p, q ), the covering space contains p copies of each observer, i.e., the covering space can be viewed as being tiled with each tile having a clone of each observer. Studies originally based on the WMAP [33] and later on higher-resolution maps from the Planck satellite [16] confirmed that there are no matched-circle pairs in the CMB sky maps. This non-detection of circles in the CMB sky can be used to constrain the lens-space parameters p and q . A lens space can conservatively be ruled out if all observers would see matched circle pairs. For the inhomogeneous lens spaces (those with q > 1) this requires comparing d LSS to the distance of every observer's nearest clone.  \nThe distance (on the unit S 3 ) between an observer at x (0) and the position of one of their clones x ( j ) given by (2.3) is 9  \nd ( p,q ) j ( s ) ≡ d ( p,q ) 0 j ( s ) = cos -1 [ s cos ( 2 πj p ) +(1 -s ) cos ( 2 πjq p )] , (3.1)  \nfor s ≡ ( x (0) 0 ) 2 +( x (0) 1 ) 2 . Notice that for the homogeneous lens space L ( p, 1) the distance to all clones is the same for all observers  \nd ( p, 1) j ( s ) = cos -1 [ s cos ( 2 πj p ) +(1 -s ) cos ( 2 πj p )] = 2 πj p . (3.2)  \n/negationslash  \nOn the other hand, since the lens spaces L ( p, q = 1) are globally inhomogeneous, the pattern of clones depends on the observer location. 10 Thus to apply the circle search limits to a topology we must search over all observers and find the maximum distance to their nearest clone. In other words, we must determine the maximum-minimum distance  \nd ( p,q ) max = max 0 ≤ s ≤ 1 ( min 0 <j<p d ( p,q ) j ( s ) ) . (3.3)  \nWe immediately see that in the homogeneous lens spaces  \nd ( p, 1) max = 2 π p . (3.4)  \nFor the inhomogeneous lens spaces ( q > 1) we compute d ( p,q ) max numerically. 11  \n9 The distance between any pair of clones x ( i ) and x ( j ) is  \nd ( p,q ) ij = cos -1 ( x ( i ) · x ( j ) ) = cos -1 [ s cos(2 π ( i -j ) /p ) + (1 -s ) cos(2 π ( i -j ) q/p )] .  \n10 The shape of the Dirichlet domain-the set of all points closer to a given observer than to any clone of that observer-also depends on the observer location for q = 1.  \n/negationslash  \nFigure 1 . The maximum-minimum distance (3.3) for each lens space L ( p, q ). Each black dot represents a different lens space. The smallest distance for each p (lower, green, dashed line) is for the homogeneous spaces L ( p, 1) given in (3.4). The maximum for each p (upper, orange, solid line) is an empirical limit (3.5) valid for all p < 8192. For illustration the distances d ( p, 11) max are shown in blue.  \n<!-- image -->  \nThe maximum-minimum distance for all lens spaces L ( p, q ) with p < 8192 is shown in Fig. 1. The smallest distance (lower, green, dashed line) occurs for the homogeneous lens spaces L ( p, 1) from (3.4). For q > 1 the distances appear to approach a maximum value with a shallow fall-off with respect to p . Empirically, it is found to be well approximated as  \nd ( p,q ) max < 2 πα √ p , (3.5)  \nwith α /similarequal 0 . 761. This choice for α is valid for all p < 8192, but appears to be increasing very little if at all by the time p reaches this value. This bound is shown as the upper, orange, solid line in the figure.  \nThe scaling of this upper limit on d ( p,q ) max as p -1 / 2 is a direct consequence of our earlier observation that R j pq keeps both x 2 0 + x 2 1 and x 2 2 + x 2 3 unchanged. This implies that the p clones of any point populate a 2-torus in R 4 (that of course lies on the S 3 ). If they are randomly distributed, then their average separation is proportional to p -1 / 2 . An analytic calculation of α seems possible. A first estimate is obtained by noting that the mean separation of p points uniformly distributed on the maximum-area 2-torus submanifold of the 3-sphere is d = √ 8 π/p , assuming that p is large enough for the areas of discs of this diameter to be well-approximated by πd 2 / 4. This leads to an estimate of α /similarequal √ 2 /π /similarequal 0 . 798, which is within a few percent of the value derived numerically.  \nThe figure also contains other noticeable band-like structure. At first glance, since the lower bound is given by d ( p, 1) max it may be thought that the bands represent other fixed values of q . This is not the case. An illustrative example for q = 11 is provided in the figure as blue dots. Though the structure is intriguing, and more prominent as one zooms into the figure, it has no bearing on the limits presented in this work and will not be explored further here.", '4 Cosmological settings': "In order to use (3.5) to constrain the topology of S 3 manifolds from cosmological data, we recall certain facts about a positively curved FLRW universe. The spherical FLRW geometry is characterized by the locally homogeneous and isotropic FLRW metric  \nd s 2 = -c 2 d t 2 + a ( t ) 2 (d χ 2 +sin 2 χ dΩ 2 ) . (4.1)  \nHere, t is the cosmic time, a ( t ) is the scale factor, χ is the comoving radial distance in units of the curvature radius R c for the 3-sphere, and dΩ 2 = d θ 2 +sin 2 θ d ϕ 2 is the infinitesimal solid angle.  \nThe first Friedmann equation in this geometry for a universe filled with homogeneous dust of density ρ (and zero pressure) and with cosmological constant Λ is  \nH ( t ) 2 = 8 πGρ ( t ) 3 -c 2 a ( t ) 2 R 2 c + Λ c 2 3 , (4.2)  \nwhere H ( t ) = ˙ a ( t ) /a ( t ) is the Hubble expansion rate, G is Newton's constant, and we have displayed R c explicitly. It is convenient to rewrite this in terms of density parameters today: Ω m for matter, Ω Λ for the cosmological constant, and Ω K as an effective density parameter for curvature, all defined by  \nΩ m ≡ 8 πGρ 0 3 H 2 0 , Ω Λ ≡ Λ c 2 3 H 2 0 , Ω K ≡ -c 2 R 2 c H 2 0 . (4.3)  \nHere all quantities are written in terms of their values today at time t 0 : H 0 ≡ H ( t 0 ), ρ 0 ≡ ρ ( t 0 ), and we have chosen a 0 ≡ a ( t 0 ) = 1. Noting that ρ ( t ) = ρ 0 /a ( t ) 3 for nonrelativistic matter we can, as usual, rewrite Eq. (4.2) as  \nH 2 = ( ˙ a a ) 2 = H 2 0 ( Ω m a -3 +Ω K a -2 +Ω Λ ) . (4.4)  \nNotice that from the definition of Ω K the current physical curvature radius is  \nR phys c ≡ a 0 R c = c H 0 √ | Ω K | . (4.5)  \nThe comoving distance between an observer and a point at redshift z can be found by using a = 1 / (1 + z ) and integrating along a radial null geodesic  \nd χ = c d t a = c d a a ˙ a = -c ( a ˙ a ) d z. (4.6)  \nFinally, using Eq. (4.4), the comoving distance in units of R c is given by  \nχ ( z ) = ∫ d χ = √ | Ω K | ∫ z 0 d x √ Ω m (1 + x ) 3 +Ω K (1 + x ) 2 +Ω Λ . (4.7)  \nAs we use CMB data to constrain topology we are interested in the diameter of the LSS, which we take to be at z LS = 1090. The comoving diameter of the LSS in units of R c is thus  \nd LSS = 2 χ ( z LS ) . (4.8)  \n<!-- image -->  \nFigure 2 . Implications of cosmology. Panel (a) on the left shows d LSS (in units of R c ) as a function of Ω K for z = 1090 and Ω m satisfying the best-fit constraint in Eq. (4.9). Panel (b) on the right shows how this, coupled with the non-observation of matched circles in the sky, imposes constraints on allowed lens spaces. The solid line is our limit p ∗ in (5.3). The shaded region (below the line) shows the values of p consistent with the non-observation of circles in the sky (with f O = 1).  \n<!-- image -->  \nThe value of d LSS given in (4.7) depends on cosmological parameters Ω m and Ω K . 12 The best-fit cosmological model from the CMB has a degeneracy between Ω m and Ω K . To approximate this degeneracy we note from Planck 2018 [34], Fig. 29, that the constraints on Ω m as a function of Ω K from primary CMB anisotropies (i.e., without lensing and baryon acoustic oscillations) are quite tight, allowing us to find an empirical relationship from the central contour in the Ω m -Ω K plane,  \nΩ m /similarequal 0 . 314 -3 . 71Ω K . (4.9)  \nBased on this relation, d LSS versus Ω K in units of R c is calculated and shown in Fig. 2. However, it should also be noted that both the location of the central contour and the tightness of the fit to (4.9) were obtained in the context of the specific power spectra adopted by Planck , which may very well require modification in the context of non-trivial topology, especially on large scales.", '5 Cosmological constraints on detectability of lens spaces': 'To combine the previous two sections, we use the condition that all observers in a lens space will see circles in the sky when  \nd ( p,q ) max < f O d LSS . (5.1)  \nf O d LSS is the observational lower limit, from the CMB, on the length of the shortest closed spatial geodesic. As discussed in Section 1, f O /similarequal 0 . 985 at 95% confidence level, but is not much smaller at much higher confidence [22]. Coupled with the upper limit on d ( p,q ) max from (3.5), this can be used to rule out lens spaces with too small distances to the nearest clone.  \nFigure 3 . The maximum-minimum clone separation in units of R c , d ( p,q ) max (from Eq. (3.3)), for all lens spaces L ( p, q ) with p < 8192. The color represents the magnitude of the distance in units of the curvature radius R c . This distance has been converted (for the empirical relationship (4.9)) to a minimum allowed value of Ω K (in square brackets) by equating d ( p,q ) max to d LSS , which is the minimum interclone distance given the non-observation of matched circles in the CMB sky.  \n<!-- image -->  \nEvery observer in the lens space L ( p, q ) will see circles if  \n2 πα √ p < f O d LSS . (5.2)  \nSolving for p and inverting the logic, the only lens spaces consistent with the non-detection of matched circles in the sky have  \np < 4 π 2 α 2 f 2 O d 2 LSS ≡ p ∗ . (5.3)  \nWe shall take f O = 1 for illustrative purposes in our figures, since our topology limits are already subject to some uncertainty due to their dependence on cosmological parameters. The value of d LSS depends on cosmological parameters (e.g., Eqs. (4.7) and (4.8)) and can be reduced to a function of Ω K using the approximation in Eq. (4.9). The resulting dependence is shown in the left panel (a) of Fig. 2. It thus follows that the bound set by p ∗ is also a function of Ω K . The parameter space of lens spaces as a function of Ω K is shown in the right panel (b) of Fig. 2 with the bound from (5.3) as a consequence of the absence of matched circles in the CMB. The white region represents the region of the parameter space (Ω K , p ) excluded for any valid choice of q , while the shaded region represents the allowed parameters for some q . Recall that precise limits on ( p, q ) depend on the specific values of cosmological parameters.  \nWe note that the parameter space allowed by the lack of matched circles, although much better constrained, is still large. These spaces are inhomogeneous for q > 1 and could therefore be observed or constrained by their effect on cosmological observables such as the CMB anisotropies; we will study their exact effect in an upcoming paper.  \nAs noted in the introduction, observational constraints on lens spaces had been considered in Ref. [27] prior to searches for circles in the sky. When applied to the LSS, that work provides an alternative and q -dependent upper bound on allowed lens spaces. They required  \n2 πq p < f O d LSS , (5.4)  \nwhich translates into the upper bound  \np < 2 πq f O d LSS ≡ p ∗ q . (5.5)  \nThe tightest constraint on lens spaces is determined from a combination of these two bounds. No observer will see circles when  \nmin ( 2 πα √ p , 2 πq p ) > f O d LSS , (5.6)  \nwhere the first distance corresponds to the bound p ∗ and the second to p ∗  \nFrom this we see that p in (5.3) provides a stricter bound than p q in (5.5) when  \nq . ∗ ∗  \nq > α √ p. (5.7)  \nThe connections between the maximum-minimum distance and cosmological data, as embodied in the curvature through Ω K , for each lens space L ( p, q ) is summarized in Fig. 3. The color represents the minimum value of d LSS for which some observers in L ( p, q ) would see circles. For any value of d LSS less than this, some observers would see circles. For any value of d LSS larger than this, no observers would see circles . The black line separates the space into regions where the bound from Ref. [27] in (5.5) on the distance is tighter (below the line) and the bound from this work in (5.3) is tighter (above the line), with the transition happening when q = α √ p . This result is independent of cosmology.  \nAdditionally, the color can also be interpreted as giving a lower limit on the value of Ω K (given in square brackets) for each lens space consistent with the non-detection of pairs of matched circles in the CMB sky. The quoted cosmology-dependent value of Ω K is computed by requiring d ( p,q ) max = d LSS (Ω K ) for the fit (4.9) to Planck 2018 cosmological data, as shown in panel (a) of Fig. 2. Again we stress that the d LSS limit (5.6) is independent of the specific values of cosmological parameters (and the details of power spectrum), whereas the Ω K limit displayed in Fig. 3 is not.', '6 Conclusions': 'The local geometry of the Universe is nearly flat, which means that it is consistent with a small, positive (or negative), isotropic 3-curvature [35]. However, positive curvature does not imply that the topology is necessarily that of the covering space of spherical geometry, S 3 . The 3-sphere admits a countable infinity of other topologies, among them the lens spaces L ( p, q ), which are quotients of S 3 by Z p , the cyclic group of order p . The integer parameter q  \n(with 0 < q < p ) indexes different realizations of such quotients (cf., Eq. (2.2)), though not all values of q in this range give manifolds, and not all values that do give manifolds are distinct, either topologically or physically.  \nAll manifolds with S 3 local geometry, and in particular all lens spaces, are compact, and the larger p is, the smaller the volume of the space for fixed curvature radius R c . Meanwhile, independent analyses of both WMAP and Planck temperature data have shown us that the shortest closed distance around the Universe through our location is greater than f O = 98 . 5% of the diameter of the last-scattering surface, d LSS (as remarked above, we take f O = 1 rather than 0 . 985 for simplicity). For fixed values of R c , this places an upper limit on p and more specifically restricts the values of ( p, q ) according to (5.6). We have shown that this limit on ( p, q ) is considerably more stringent than the previous limit (5.5) for most values of ( p, q ). In Fig. 3, we have presented this limit, giving cosmology-independent values of the maximum-minimum clone separation in units of R c , d ( p,q ) max , and (in square brackets) cosmology-dependent values of the maximum allowed value of Ω K given the empirical relation (4.9) obtained from the primary CMB anisotropies measured by Planck [34].  \nFuture work will extend these limits to the other S 3 topologies: the prism manifolds (a.k.a. dihedral spaces), and the tetrahedral, octahedral, and icosahedral spaces. We will also present the spin-0 and spin-2 eigenmodes of spherical geometries, and the correlation matrices of density and CMB fluctuations of all types, allowing us to predict the statistical properties of the CMB and of other cosmological observables in all S 3 manifolds.', 'Acknowledgments': "S.S., C.J.C., and G.D.S. thank D. Singer for extended conversations about the geometry and topology of S 3 manifolds. We thank J. Weeks for several valuable conversations. This work made use of the High-Performance Computing Resource in the Core Facility for Advanced Research Computing at Case Western Reserve University. Y.A. acknowledges support by the Spanish Research Agency (Agencia Estatal de Investigación)'s grant RYC2020-030193I/AEI/10.13039/501100011033, by the European Social Fund (Fondo Social Europeo) through the Ramón y Cajal program within the State Plan for Scientific and Technical Research and Innovation (Plan Estatal de Investigación Científica y Técnica y de Innovación) 2017-2020, and by the Spanish Research Agency through the grant IFT Centro de Excelencia Severo Ochoa No CEX2020-001007-S funded by MCIN/AEI/10.13039/501100011033. T.S.P. acknowledges financial support from the Brazilian National Council for Scientific and Technological Development (CNPq) under grants 312869/2021-5 and 88881.709790/2022-0. C.J.C., G.D.S., A.K., and D.P.M. acknowledge partial support from NASA ATP grant RES240737; G.D.S. and Y.A. from the Simons Foundation; G.D.S. and A.S. from DOE grant DESC0009946; G.D.S., Y.A., and A.H.J. from the Royal Society (UK); and A.H.J. from STFC in the UK. A.T. is supported by the Richard S. Morrison Fellowship. G.D.S. and Y.A. thank the INFN (Sezione di Padova), and G.D.S., S.A., D.P.M., and A.T. thank the IFT for hospitality where part of this work was accomplished.", 'References': "- [1] A. Einstein, 'The foundation of the general theory of relativity.,' Annalen Phys. 49 no. 7, (1916) 769-822.  \n- [2] COMPACT Collaboration, A. Samandar et al. , 'Cosmic topology. Part IIIa. Microwave background parity violation without parity-violating microphysics,' arXiv:2407.09400 [astro-ph.CO] .\n- [3] J. Jones, C. J. Copi, G. D. Starkman, and Y. Akrami, 'The Universe is not statistically isotropic,' arXiv:2310.12859 [astro-ph.CO] .\n- [4] Planck Collaboration, P. A. R. Ade et al. , 'Planck 2013 results. XXIII. Isotropy and statistics of the CMB,' Astron. Astrophys. 571 (2014) A23, arXiv:1303.5083 [astro-ph.CO] .\n- [5] D. J. Schwarz, C. J. Copi, D. Huterer, and G. D. Starkman, 'CMB Anomalies after Planck,' Class. Quant. Grav. 33 no. 18, (2016) 184001, arXiv:1510.07929 [astro-ph.CO] .\n- [6] Planck Collaboration, P. A. R. Ade et al. , 'Planck 2015 results. XVI. Isotropy and statistics of the CMB,' Astron. Astrophys. 594 (2016) A16, arXiv:1506.07135 [astro-ph.CO] .\n- [7] Planck Collaboration, Y. Akrami et al. , 'Planck 2018 results. VII. Isotropy and Statistics of the CMB,' Astron. Astrophys. 641 (2020) A7, arXiv:1906.02552 [astro-ph.CO] .\n- [8] E. Abdalla et al. , 'Cosmology intertwined: A review of the particle physics, astrophysics, and cosmology associated with the cosmological tensions and anomalies,' JHEAp 34 (2022) 49-211, arXiv:2203.06142 [astro-ph.CO] .\n- [9] A. Einstein, 'Cosmological Considerations in the General Theory of Relativity,' Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys.) 1917 (1917) 142-152.\n- [10] W. de Sitter, 'On Einstein's Theory of Gravitation and its Astronomical Consequences. Third Paper.,' Mon. Not. Roy. Astron. Soc. 78 no. 1, (1917) 3-28.\n- [11] R. Lehoucq, M. Lachieze-Rey, and J. P. Luminet, 'Cosmic crystallography,' Astron. Astrophys. 313 (1996) 339-346, arXiv:gr-qc/9604050 .\n- [12] N. J. Cornish, D. N. Spergel, and G. D. Starkman, 'Circles in the sky: Finding topology with the microwave background radiation,' Class. Quant. Grav. 15 (1998) 2657-2670, arXiv:astro-ph/9801212 .  \n[13] N. J. Cornish, D. N. Spergel, and G. D. Starkman, 'Measuring the topology of the universe,'  \nProc. Nat. Acad. Sci.  \n95  \n(1998) 82,  \narXiv:astro-ph/9708083  \n.  \n- [14] N. J. Cornish, D. N. Spergel, G. D. Starkman, and E. Komatsu, 'Constraining the topology of the universe,' Phys. Rev. Lett. 92 (2004) 201302, arXiv:astro-ph/0310233 .\n- [15] M. Kunz, N. Aghanim, L. Cayon, O. Forni, A. Riazuelo, and J. P. Uzan, 'Constraining topology in harmonic space,' Phys. Rev. D 73 (2006) 023511, arXiv:astro-ph/0510164 .\n- [16] Planck Collaboration, P. A. R. Ade et al. , 'Planck 2013 results. XXVI. Background geometry and topology of the Universe,' Astron. Astrophys. 571 (2014) A26, arXiv:1303.5086 [astro-ph.CO] .\n- [17] Planck Collaboration, P. A. R. Ade et al. , 'Planck 2015 results - XVIII. Background geometry and topology of the Universe,' Astron. Astrophys. 594 (2016) A18, arXiv:1502.01593 [astro-ph.CO] .\n- [18] COMPACT Collaboration, Y. Akrami et al. , 'Promise of Future Searches for Cosmic Topology,' Phys. Rev. Lett. 132 no. 17, (2024) 171501, arXiv:2210.11426 [astro-ph.CO] .\n- [19] COMPACT Collaboration, P. Petersen et al. , 'Cosmic topology. Part I. Limits on orientable Euclidean manifolds from circle searches,' JCAP 01 (2023) 030, arXiv:2211.02603 [astro-ph.CO] .\n- [20] COMPACT Collaboration, J. R. Eskilt et al. , 'Cosmic topology. Part IIa. Eigenmodes, correlation matrices, and detectability of orientable Euclidean manifolds,' JCAP 03 (2024) 036, arXiv:2306.17112 [astro-ph.CO] .  \n- [21] COMPACT Collaboration, A. Tamosiunas et al. , 'Cosmic topology. Part IVa. Classification of manifolds using machine learning: a case study with small toroidal universes,' arXiv:2404.01236 [astro-ph.CO] .\n- [22] P. M. Vaudrevange, G. D. Starkman, N. J. Cornish, and D. N. Spergel, 'Constraints on the Topology of the Universe: Extension to General Geometries,' Phys. Rev. D 86 (2012) 083526, arXiv:1206.2939 [astro-ph.CO] .\n- [23] J. Shapiro Key, N. J. Cornish, D. N. Spergel, and G. D. Starkman, 'Extending the WMAP Bound on the Size of the Universe,' Phys. Rev. D 75 (2007) 084034, arXiv:astro-ph/0604616 .\n- [24] P. M. Vaudrevange, G. D. Starkman, N. J. Cornish, and D. N. Spergel. Private Communication, 2013.\n- [25] W. P. Thurston, 'Three dimensional manifolds, kleinian groups and hyperbolic geometry,' Bulletin of the American Mathematical Society 6 (1982) 357-381.\n- [26] E. Gausmann, R. Lehoucq, J.-P. Luminet, J.-P. Uzan, and J. Weeks, 'Topological lensing in spherical spaces,' Class. Quant. Grav. 18 (2001) 5155-5186, arXiv:gr-qc/0106033 .\n- [27] G. I. Gomero, M. J. Reboucas, and R. K. Tavakol, 'Detectability of cosmic topology in almost flat universes,' Class. Quant. Grav. 18 (2001) 4461-4476, arXiv:gr-qc/0105002 .\n- [28] J.-P. Uzan, A. Riazuelo, R. Lehoucq, and J. Weeks, 'Cosmic microwave background constraints on lens spaces,' Phys. Rev. D 69 (2004) 043003, arXiv:astro-ph/0303580 .\n- [29] R. Aurich, P. Kramer, and S. Lustig, 'CMB radiation in an inhomogeneous spherical space,' Phys. Scripta 84 (2011) 055901, arXiv:1107.5214 [astro-ph.CO] .\n- [30] R. Aurich and S. Lustig, 'How well-proportioned are lens and prism spaces?,' Class. Quant. Grav. 29 (2012) 175003, arXiv:1201.6490 [astro-ph.CO] .\n- [31] R. Aurich and S. Lustig, 'A survey of lens spaces and large scale CMB anisotropy,' Mon. Not. Roy. Astron. Soc. 424 (2012) 1556-1562, arXiv:1203.4086 [astro-ph.CO] .\n- [32] W. Threlfall and H. Seifert, 'Topologische untersuchung der diskontinuitätsbereiche endlicher bewegungsgruppen des dreidimensionalen sphärischen raumes,' Mathematische Annalen 104 (1931) 1-70. http://eudml.org/doc/159448 .\n- [33] R. Aurich and S. Lustig, 'A search for cosmic topology in the final WMAP data,' Mon. Not. Roy. Astron. Soc. 433 (2013) 2517, arXiv:1303.4226 [astro-ph.CO] .\n- [34] Planck Collaboration, N. Aghanim et al. , 'Planck 2018 results. VI. Cosmological parameters,' Astron. Astrophys. 641 (2020) A6, arXiv:1807.06209 [astro-ph.CO] . [Erratum: Astron. Astrophys. 652, C4 (2021)].\n- [35] S. Anselmi, M. F. Carney, J. T. Giblin, S. Kumar, J. B. Mertens, M. O'Dwyer, G. D. Starkman, and C. Tian, 'What is flat ΛCDM, and may we choose it?,' JCAP 02 (2023) 049, arXiv:2207.06547 [astro-ph.CO] ."}