Issue 
A&A
Volume 540, April 2012



Article Number  A29  
Number of page(s)  5  
Section  Cosmology (including clusters of galaxies)  
DOI  https://doi.org/10.1051/00046361/201117845  
Published online  20 March 2012 
Research Note
A coordinateindependent technique for detecting globally inhomogeneous flat topologies
Institute of Astronomy, School of Science, University of Tokyo, 2211, Osawa, Mitaka, 1810015 Tokyo, Japan
email: hfujii@ioa.s.utokyo.ac.jp
Received: 8 August 2011
Accepted: 6 February 2012
A flat Universe model that is supported by recent observations can choose among 18 possibilities for its overall topology. To detect or exclude these possibilities is one of the most important tasks in modern cosmology, but it has been very difficult to make for globally inhomogeneous models because of the long time needed for the calculation. In this brief paper we provide an objectbased 3D method to overcome the problem, as an extension of Fujii & Yoshii (2011, A&A, 529, A121). Though the test depends on the observer’s location in the universe, this method drastically reduces calculation times to constrain inhomogeneous topologies, and will be useful in exhaustively constraining the size of the flat Universe.
Key words: largescale structure of Universe / cosmology: theory
© ESO, 2012
1. Introduction
The theory of modern cosmology is based on Einstein’s general relativity, and recent observations favor a ΛCDM cosmology with vanishing curvature (e.g., from WMAP+BAO+SN data, by Jarosik et al. 2011), which successfully describes the observed properties such as the cosmic structure formation, the cosmic microwave background (CMB) anisotropies, and the accelerating expansion. However, General Relativity does not distinguish between two spaces with the same curvature but with different topologies. Though the curvature of our Universe is exactly zero, we still have 18 choices for the overall topology of the Universe (Nowacki 1934), e.g., the multiconnected threetorus T^{3} with finite volume. Of these 18 choices, however, 8 topologies are nonorientable and are usually regarded to be physically unacceptable because of arguments of the CPT invariance (LachièzeRey & Luminet 1995).
A multiconnected space is a quotient space of the simply connected space with the same curvature (S^{3}, E^{3}, or H^{3}, called covering space), by a holonomy group Γ. It is imagined as a finite or infinite 2Kpolyhedron (the Dirichlet domain), whose K pairs of surfaces are connected by the holonomies. Because of these compact dimensions there are many geodesics that connect a given object and the observer, which implies multiple images of single objects, often referred to as “ghosts” (for details, see, e.g., LachièzeRey & Luminet 1995). As a result, an observer sees the covering space tessellated by polyhedra (“ghosts” of the Dirichlet domain).
Based on this prediction, many objectbased works for exploring cosmic topology were carried out, i.e., one searched for periodic and symmetrical patterns made by ghosts of galaxies, galaxy clusters, or active galactic nuclei (e.g., Sokolov & Shvartsman 1974; Fagundes & Wichoski 1987; Demiański & Łapucha 1987; Lehoucq et al. 1996; Roukema 1996; Uzan et al. 1999; Weatherley et al. 2003; Marecki et al. 2005; Menzies & Mathews 2005; Fujii & Yoshii 2011a,b). Owing to the lack of highredshift data, objectbased methods are normally not suitable for constraining the size of the Universe.
The recent trend is to use CMB data that have the highest redshift available, z ≃ 1100. The circlesinthesky method (Cornish et al. 1998) is a direct method of searching for ghosts of CMB: intersections of the lastscattering surface and our Dirichlet domain. They appear as circles with the same temperature fluctuation pattern in a CMB map since they are physically identical. This method can detect any topologies, but checking all possibilities requires an extremely longtime calculation because of many free parameters: the radius of the matched circles, the celestial positions of centers of the two circles, and the relative phase between the two. The parameter space, however, can be somewhat reduced using the results by Mota et al. (2011).
Exhaustive analyses have not been carried out yet, and various authors searched for matched circles in data limited to antipodal or nearly antipodal ones, using the WMAP satellite’s data. Some authors found hints of specific topologies (Poincaré dodecahedral space by Roukema et al. 2008; cubic threetorus by Aurich 2008), while others found no detection and obtained the lower limit of the size of our Universe (Cornish et al. 2004; Key et al. 2007; Bielewicz & Banday 2011). The most recent one is ≥ 27.9 Gpc by Bielewicz & Banday (2011), which is consistent with the results by Aslanyan & Manohar (2011), who indirectly constrained compact dimensions for three topologies, T^{3},T^{2} × R^{1}, and S^{1} × R^{2}, using CMB statistics. These discrepancies could be caused by the methodological problems or by the quality of the CMB map: the signal may be blurred by Doppler, SachsWolfe, or integrated SachsWolfe effects because of the coarse resolution.
Despite the above mentioned results, the possibility that we live in a small universe still remains, because no detection of antipodal (or nearly antipodal) circles puts weaker constraints on the size of inhomogeneous spaces (see Sect. 2.1), e.g., ≥ 28/3 = 9.3 Gpc for a thirdturn space topology and ≥28/4 = 7 Gpc for a quarterturn space topology. These scales can be explored using lowredshift (compared to CMB) cosmic objects. In the previous paper we developed an objectbased method that can constrain any of the 18 flat topologies with simple algorithms, and is much more sensitive to topological signatures than the preceding ones (Fujii & Yoshii 2011a, hereafter FY11a). Unfortunately, it has a similar problem in checking all possible topologies: calculation times become very long. The aim of this brief paper is to provide a technique, which is valid under some conditions, to overcome the problem. Throughout the paper we consider flat universes, and the calculations were made in comoving coordinates.
2. Method
2.1. Mathematical background and definitions
The mathematical classification of the holonomy groups for flat spaces was completed by Nowacki (1934). Any holonomy γ can be written as γ = γ_{T}γ_{NT}, where γ_{T} is a parallel translation and γ_{NT} is an identity, nth turn rotations (for n = 2,3,4, or 6), or a reflection. Those spaces whose holonomy groups include only translations (γ_{NT} = id) are called (globally) homogeneous, all others are called (globally) inhomogeneous. We investigate the latter topologies in this paper.
We write the holonomies in a convenience way using a 4D coordinate system (w,x,y,z) where the simply connected threeEuclidean space E^{3} is represented as a hyperplane w = 1, so that a usual 3D vector (x,y,z) is represented as a 4D vector x = (1,x,y,z). Every holonomy γ is also written as a 4 × 4 matrix, e.g., a quarterturn corkscrew motion is written as
where U is a 4 × 4 matrix representing the choices of the coordinate systems, which reduces to U = id if we choose our zaxis to be parallel to the rotational axis. Hereafter we call this straight line the fundamental axis of the holonomy, denoted by l_{fun}. The unit vector n_{fun} that is parallel to l_{fun} is called the fundamental vector; we identify two antipodal vectors n_{fun} and − n_{fun}. For a glide reflection, the fundamental axis l_{fun} is defined to be parallel to the reflectional plane.
In this paper, we continue to consider the same quarterturn corkscrew motion as an example.
2.2. Summary of the 3D method of FY11a
We review here the FY11a objectbased 3D method for detecting cosmic topology (see the paper for details). Our assumption is that the Universe has a spatial section with zero curvature, as suggested by recent observations.
If a pair of comoving objects x_{1} and are linked by a holonomy γ, we have by definition (1)where L = (1,L_{1},L_{2},L_{3}) is the translational vector. Detecting these topological twins requires a parameter search for five parameters: the translational vector L counts for three and the fundamental vector n_{fun} counts for two. To eliminate L, we search for two pairs of ghosts (called a topological quadruplet) )] such that Such a quadruplet always satisfies (4)independent of L. If our zaxis is parallel to the fundamental axis l_{fun} (hence U = id), the following relations hold: since γ is a quarterturn corkscrew motion here.
The FY11a scheme is to search for quadruplets [(x_{i},x_{j}),(x_{k},x_{l})] that simultaneously satisfy the following three conditions:

1.
Separation condition: x_{i} − x_{j} = x_{k} − x_{l}.

This condition is common to all holonomies, because holonomies are isometries that preserve distance. Preceding works such as Roukema (1996) and Uzan et al. (1999) also used this mathematical property of holonomies.

2.
Vectorial condition: Eqs. (5)–(7).

This is for a quarterturn corkscrew motion; for other types of holonomies, see FY11a. A similar condition for a translation was used in Marecki et al. (2005).

3.
Lifetime condition: t_{i} − t_{k},t_{j} − t_{l} < t_{life}.

The variables t_{i},t_{j},... are cosmic times of objects x_{i},x_{j},··· , respectively, and t_{life} is the typical lifetime of objects. This condition is important when considering shortlived objects, e.g., active galactic nuclei.
Because of these multifilters, only few ghosts qualify for this test. However, Eqs. (5)–(7) holds only for the specific coordinate system, so we still have to perform the parameter search for two parameters, the fundamental vector n_{fun}. To our dismay, this requires more than 10^{6} trials, which takes a very long time, since the typical value of the peculiar velocity is 500 km s^{1}, the quasar lifetime is 10^{8} yr, and their distance ~Gpc implies an angular positional uncertainty of ~10^{3}. These strong and weak points of the FY11a method is seen in Fig. 1. The integer s is assigned to each object, which is the number of quadruplets including the object as a member, which satisfies all conditions 1–3 (see FY11a for details); topologically lensed objects tend to have high s values. When using the zaxis parallel to n_{fun}, some bumps in the histograms are seen that are produced by topological ghosts, while these bumps are not seen when the zaxis deviates from n_{fun}. The property of the simulated catalog used here is described in Sect. 3.1.
Fig. 1
Solid line: the result using the zaxis parallel to n_{fun}. Broken line: the result using the zaxis that is at an angle of π/6 with n_{fun}. The catalog used here consists of 1008 objects including 10 pairs of ghosts, and the observer stands at a distance of 1.75 Gpc from l_{fun} (see Sect. 3.2). Vertical scale is linear from 0 to 1 and logarithmic from 1 to 1000. 
2.3. Fundamentalvectorsearching method
One may aim to have a coordinateindependent filter to extract topological quadruplets, but we found this to be impossible. Consider a quadruplet [(x_{i},x_{j}),(x_{k},x_{l})] that already satisfies the separation condition and the lifetime condition. It then also satisfies the vectorial condition Eqs. (5)–(7) if we choose the zaxis parallel to a vector n_{pec}, seen along which the two vectors a = x_{j} − x_{i} and b = x_{l} − x_{k} make a right angle (Fig. 2). The unit vector n_{pec} is called peculiar vector of the quadruplet, for a quarterturn corkscrew motion.
Fig. 2
Even a nontopological quadruplet seems to be linked by a quarterturn corkscrew motion when we choose the zaxis parallel to its peculiar axis n_{pec}. 
We consider the quarterturn corkscrew motion as an example throughout the paper, but treatments of the other types of holonomies are the same except for the step 3. The peculiar axis of the quadruplet [(x_{i},x_{j}),(x_{k},x_{l})] for each type of holonomies can be defined as follows.
1. Nth turn corkscrew motions. In this case the fundamental axis is defined to be parallel to the rotational axis. The apparent angle between a and b, therefore, should be 2π/n when seen from its peculiar vector n_{pec}. This vector is obtained by rotating the unit vector parallel to a + b around the axis parallel to a − b by the angle of (8)where φ is half the intrinsic angle between a and b. The quadruplet with φ > π/n has no peculiar axes, which never occurs when n = 2 (halfturn corkscrew motion).
2. Glide reflections. In this case the fundamental axis is defined to be perpendicular to the reflectional plane, hence the peculiar vector is the unit vector parallel to a − b.
Therefore, it is impossible to judge whether a given quadruplet is topological, however, if there really exists a fundamental axis (and vector) in the Universe, there should be more quadruplets whose peculiar vectors are parallel to it than stochastically expected. To detect such an excess alignment is the essential idea of the coordinateindependent technique described here. The detailed procedure, which hereafter we call the “fundamentalvectorsearching (FVS)” method, works as follows.

1.
The celestial sphere is divided into equal area pixels. Because we identify two antipodal vectors, the number of pixels used is .

2.
The quadruplets that satisfy both the separation condition and the lifetime condition are selected.

3.
For each selected quadruplet, its peculiar vector n_{pec} and the pixel containing n_{pec} within it is calculated.

4.
For each object x_{i}, we flag pixels that contain more than s_{min} peculiar axes of the quadruplets that include x_{i}.

5.
Each pixel is assigned an integer with the number of times that it was flagged in the previous step.
These steps practically correspond to counting the number of objects with s_{i} > s_{min} for all possible zaxes. Note that the choices of the parameters N_{side} and s_{min} are not independent; a small N_{side} corresponds to large pixels and large stochastic noises, so s_{min} should be chosen to be large enough. We used the HEALPix scheme (Górski et al. 2005) for the pixelization of the celestial sphere.
3. Simulations and discussions
3.1. Details of simulated catalogs
To demonstrate how the FVS method works, we applied the method to catalogs of toy quasars. The details of the simulations are as follows.

The standard ΛCDM cosmology (Ω_{m} = 0.27,Ω_{Λ} = 0.73,H_{0} = 71 km s^{1} Mpc^{1}) was used so that the local geometry is Euclidean.

A quarterturn space topology was assumed such that the detectable holonomies are only two quarterturn corkscrew motions. The translational distance of these detectable holonomies is L = 7 Gpc, which is consistent with the negative results on homogeneous topologies using the WMAP data (see Sect. 1).

We used a full sky and shelllike catalog: 3.5 Gpc (L/2) < r < 5.25 Gpc (3L/4) in comoving radius, or 1.1 ≲ z ≲ 2.0 in redshift.

The objects are distributed uniformly in the comoving space.

The quasar luminosity evolution was simplified such that they emit radiation with a constant luminosity during the fixed duration t_{life} = 10^{8} yr.

The peculiar motion was simplified to move with a constant speed v = 500 km s^{1} and with randomly chosen directions.

Other natures of quasars and technical uncertainties were all ignored.
We acknowledge that these simple assumptions are not suitable for practical applications; the aim here is just to show the essence of the test.
Fig. 3
Fundamental vector n_{fun} appears as a sharp peak in both cases; left: θ = 0, right: θ = π/6. The observer stands at a distance of 1.75 Gpc from the fundamental axis l_{fun}. 
3.2. Main results: detection of the fundamental axis
First we applied the FY11a method to a toy quasar catalog seen from an observer standing at a comoving distance of r_{obs} = 1.75 Gpc (L/4) from l_{fun}. The catalog contains 1008 objects, including 10 pairs of ghosts. Two choices of coordinate systems were used, θ = 0 and π/6, where θ is the angle between the chosen zaxis and n_{fun}. These results are given in Fig. 1 and were already discussed; the topological signal appears only for the former case (θ = 0), and we generally have to change our zaxis as free parameters to detect globally inhomogeneous topologies (see also Sect. 5.2.1 of FY11a). This takes an extremely long time, which motivated us to commence this work.
Next we applied the FVS method to the same catalog using N_{side} = 500 and s_{min} = 2. If there is a topological quadruplet, its peculiar vector n_{pec} ideally coincides with the fundamental vector n_{fun}, but not in practice because of the peculiar motions. The resolution parameter N_{side} is determined so that it covers this positional deviations. The cutoff parameter s_{min} = 2 is a reasonable choice because the quadruplets with s_{i} > 2 seem to rarely occur by chance, as can be seen in Fig. 1 (broken line).
The results are shown as 2D color histograms (Fig. 3), where half the celestial sphere is orthogonally projected onto the xyplane. As expected, a pixel containing the fundamental axis has more counts than the other pixels, whose counts are purely stochastic, independently of the coordinate systems.
This single calculation takes about a few minutes with a presentday ordinary personal computer, and is equivalent to performing about ~10^{6} trials of the FY11a method, which takes about one year. This is the notable advantage of the FVS method over the other methods, e.g., the CMBbased circlesinthesky method that cannot constrain all possible topologies in a reasonable time.
3.3. Limits of the method: observer’s location
The results of the previous section are based on somewhat idealized assumptions. In practice, there are various effects to be considered correctly: physical properties of astronomical objects and observational uncertainties. These effects will be treated in forthcoming papers and not here, but there is another important factor that affects this test; the limit of the FVS method depends on the observer’s location in the universe.
For there to be a sharp peak, the following two conditions must be satisfied:

1.
all peculiar vectorsn_{pec} of topological quadruplets are lying in one (or a few) pixel;

2.
the stochastic noise contained in one pixel is much less than the topological signal.
The first condition requires a sufficiently large pixel size, while the second condition requires a sufficiently small pixel size. Consequently, one needs to find a good balance between them, however, this becomes impossible for an observer “near” the fundamental axis l_{fun}.
Fig. 4
If the observer stands along l_{fun}, the FVS method does not work well (right) and a tremendous parameter search of the FY11a method is necessary (left). A sharp peak at (0,0) is leveled because of the high dispersion of n_{pec} of topological quadruplets. 
To see this effect, let us consider a topological quadruplet , which satisfies where a = x_{j} − x_{i}, , and ε represents the positional perturbations due to peculiar motions. The coordinate system is chosen so that the zaxis corresponds to l_{fun}. To calculate the peculiar vector of this quadruplet, we need two vectors a + b and a − b (Sect. 2.3): (12)(13)whose directions are highly perturbed from the unperturbed ones if a_{x} + a_{y},a_{x} − a_{y}, or a_{z} are comparable to ε. Indeed, a_{z} systematically takes low values if the surfaces of the Dirichlet domain are nearly perpendicular to l_{fun} when using shortlived objects such as quasars and starburst galaxies, which are luminous and suitable for highredshift observations, since their ghosts appear close to (on the order of ~ ct_{life}) the surfaces. The angle between the Dirichlet domain surface and l_{fun} is given by , so this situation occurs when r_{obs}/L ≪ 1. For such an observer it is hard to find a good compromise between the two conditions.
Therefore, if the Milky Way happens to be situated near l_{fun} compared to L, the FVS method can no longer detect topological signatures and a troublesome parameter search of FY11a method (or other possible methodologies) is needed. For example, we generated a toy quasar catalog seen from the observer standing along l_{fun}. The catalog contains 996 objects including 11 pairs of ghosts. In Fig. 4, it can be seen that the FVS method does not detect the fundamental vector, while the FY11a method successfully detects the topological signature, although in practice a prolonged calculation to search for n_{fun} is needed.
We have seen what happens when r_{obs}/L ≪ 1, however, there is another effect of the observer’s location, which is that the distance d to the Dirichlet domain surfaces is a monotonically increasing function of r_{obs} (see also Sect. 5.2.2 of FY11a). For a halfturn corkscrew motion it is given by (14)When r_{obs} is larger than a certain value the observed region is entirely contained in the Dirichlet domain, which implies no ghost images. In contrast to the former effect, in this case any other direct method, which is to search for topological ghosts, is also invalid.
3.4. Summary and prospects
We introduced an objectbased method (FVS method) that is able to enhance the lower limit on the size of the Universe for inhomogeneous flat topologies. If the Universe has a fundamental axis l_{fun} (or vector n_{fun}) and sufficiently small dimension, topological quadruplets tend to align with it, as can be seen in Fig. 3 (sharp spikes). This is a parameterfree extension of FY11a method, which treated n_{fun} as free parameters.
However, for a practical application we need more realistic simulations. Therefore our next work will focus on these problems: detailed treatments on physical properties of astronomical objects and technical uncertainties of observations. When this is accomplished, we will be able to apply the FVS method to the observed catalogs of our real Universe. Recent and future largescale survey projects, such as 2dFGRS (Croom et al. 2004), SDSS (Schneider et al. 2010), the Large Synoptic Survey Telescope (LSST), and the Joint Astrophysics Nascent Universe Satellite (JANUS) will provide sufficient data for this test. The formidable progress in techniques for measuring photometric redshifts suggests that the spectroscopic surveys are not necessarily needed, which makes the application more realistic.
Acknowledgments
I gratefully acknowledge Y. Yoshii for his various supports, useful discussions and constructive suggestions. I also thank M. Doi, T. Minezaki, T. Tsujimoto, T. Yamagata, T. Kakehata, K. Hattori, and T. Shimizu for useful discussions and suggestions. Finally, I thank the referee for careful reading of the paper and for constructive suggestions. Some of the results in this paper were derived using the HEALPix package.
References
 Aslanyan, G., & Manohar, A. V. 2011 [arXiv:1104.0015] [Google Scholar]
 Aurich, R. 2008, Class. Quant. Grav., 25, 225017 [NASA ADS] [CrossRef] [Google Scholar]
 Aurich, R., & Lustig, S. 2011, Class. Quant. Grav., 28, 085017 [NASA ADS] [CrossRef] [Google Scholar]
 Bielewicz, P., & Banday, A. J. 2011, MNRAS, 412, 2104 [NASA ADS] [CrossRef] [Google Scholar]
 Cornish, N. J., Spergel, D. N., & Starkman, G. D. 1998, Class. Quant. Grav., 15, 2657 [Google Scholar]
 Cornish, N. J., Spergel, D. N., Starkman, G. D., & Komatsu, E. 2004, Phys. Rev. Lett., 92, 201302 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Croom, S. M., Smith, R. J., Boyle, B. J., et al. 2004, MNRAS, 349, 1397 [NASA ADS] [CrossRef] [Google Scholar]
 Demianski, M., & Lapucha, M. 1987, MNRAS, 224, 527 [NASA ADS] [Google Scholar]
 Fagundes, H. V., & Wichoski, U. F. 1987, ApJ, 322, L5 [NASA ADS] [CrossRef] [Google Scholar]
 Fan, X., Strauss, M. A., Schneider, D. P., et al. 2001, AJ, 121, 54 [NASA ADS] [CrossRef] [Google Scholar]
 Fujii, H., & Yoshii, Y. 2011a, A&A, 529, A121 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Fujii, H., & Yoshii, Y. 2011b, A&A, 531, A171 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Górski, K. M., Hivon, E., Banday, A. J., et al. 2005, ApJ, 622, 759 [NASA ADS] [CrossRef] [Google Scholar]
 Ivezic, Z., Tyson, J. A., Acosta, E., et al. 2008, unpublished [arXiv:0805.2366] [Google Scholar]
 Key, J. S., Cornish, N. J., Spergel, D. N., & Starkman, G. D. 2007, Phys. Rev. D, 75, 084034 [NASA ADS] [CrossRef] [Google Scholar]
 LachiezeRey, M., & Luminet, J. 1995, Phys. Rep., 254, 135 [NASA ADS] [CrossRef] [Google Scholar]
 Lehoucq, R., LachiezeRey, M., & Luminet, J. P. 1996, A&A, 313, 339 [NASA ADS] [Google Scholar]
 Lehoucq, R., Uzan, J., & Luminet, J. 2000, A&A, 363, 1 [NASA ADS] [Google Scholar]
 Lew, B., & Roukema, B. 2008, A&A, 482, 747 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Linde, A. 2004, J. Cosmol. Astropart. Phys., 10, 4 [Google Scholar]
 Marecki, A., Roukema, B. F., & Bajtlik, S. 2005, A&A, 435, 427 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Menzies, D., & Mathews, G. J. 2005, J. Cosmol. Astropart. Phys., 10, 8 [NASA ADS] [CrossRef] [Google Scholar]
 Mota, B., Rebouças, M. J., & Tavakol, R. 2010, Phys. Rev. D, 81, 103516 [NASA ADS] [CrossRef] [Google Scholar]
 Nowacki, W. 1934, Comment. Math. Helvet., 7, 81 [CrossRef] [Google Scholar]
 Roming, P. 2008, in COSPAR, Plenary Meeting, 37th COSPAR Scientific Assembly, 37, 2645 [Google Scholar]
 Roukema, B. F. 1996, MNRAS, 283, 1147 [NASA ADS] [Google Scholar]
 Roukema, B. F., Lew, B., Cechowska, M., Marecki, A., & Bajtlik, S. 2004, A&A, 423, 821 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Roukema, B. F., Buliński, Z., & Gaudin, N. E. 2008a, A&A, 492, 657 [Google Scholar]
 Roukema, B. F., Buliński, Z., Szaniewska, A., & Gaudin, N. E. 2008b, A&A, 486, 55 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Schneider, D. P., Richards, G. T., Hall, P. B., et al. 2010, AJ, 139, 2360 [NASA ADS] [CrossRef] [Google Scholar]
 Uzan, J., Lehoucq, R., & Luminet, J. 1999, A&A, 351, 766 [NASA ADS] [Google Scholar]
 Weatherley, S. J., Warren, S. J., Croom, S. M., et al. 2003, MNRAS, 342, L9 [Google Scholar]
All Figures
Fig. 1
Solid line: the result using the zaxis parallel to n_{fun}. Broken line: the result using the zaxis that is at an angle of π/6 with n_{fun}. The catalog used here consists of 1008 objects including 10 pairs of ghosts, and the observer stands at a distance of 1.75 Gpc from l_{fun} (see Sect. 3.2). Vertical scale is linear from 0 to 1 and logarithmic from 1 to 1000. 

In the text 
Fig. 2
Even a nontopological quadruplet seems to be linked by a quarterturn corkscrew motion when we choose the zaxis parallel to its peculiar axis n_{pec}. 

In the text 
Fig. 3
Fundamental vector n_{fun} appears as a sharp peak in both cases; left: θ = 0, right: θ = π/6. The observer stands at a distance of 1.75 Gpc from the fundamental axis l_{fun}. 

In the text 
Fig. 4
If the observer stands along l_{fun}, the FVS method does not work well (right) and a tremendous parameter search of the FY11a method is necessary (left). A sharp peak at (0,0) is leveled because of the high dispersion of n_{pec} of topological quadruplets. 

In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.