Hyperbolic universes with a horned topology and the cosmic microwave background anisotropy

Aurich, R.; Lustig, Sven; Steiner, Frank; Then, Holger

doi:10.1088/0264-9381/21/21/010

Cited by 47 publications

(73 citation statements)

References 57 publications

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“…The details of the computation of the quantities needed in (24) are described in [12]. The first two terms in (24) are the ordinary Sachs-Wolfe contribution (9) discussed (a) Figure 6.…”

Section: The Spherical Space Forms and Their Vibrational Modesmentioning

confidence: 99%

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CMB anisotropy of spherical spaces

Aurich

Lustig

Steiner

2005

Class. Quantum Grav.

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128

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Abstract. The first-year WMAP data taken at their face value hint that the Universe might be slightly positively curved and therefore necessarily finite, since all spherical (Clifford-Klein) space forms M 3 = S 3 /Γ, given by the quotient of S 3 by a group Γ of covering transformations, possess this property. We examine the anisotropy of the cosmic microwave background (CMB) for all typical groups Γ corresponding to homogeneous universes. The CMB angular power spectrum and the temperature correlation function are computed for the homogeneous spaces as a function of the total energy density parameter Ω tot in the large range [1.01, 1.20] and are compared with the WMAP data. We find that out of the infinitely many homogeneous spaces only the three corresponding to the binary dihedral group T ⋆ , the binary octahedral group O ⋆ , and the binary icosahedral group I ⋆ are in agreement with the WMAP observations. Furthermore, if Ω tot is restricted to the interval [1.00, 1.04], the space described by T ⋆ is excluded since it requires a value of Ω tot which is probably too large being in the range [1.06, 1.07]. We thus conclude that there remain only the two homogeneous spherical spaces S 3 /O ⋆ and S 3 /I ⋆ with Ω tot of about 1.038 and 1.018, respectively, as possible topologies for our 98.70.Vc, 98.80.Es

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“…The details of the computation of the quantities needed in (24) are described in [12]. The first two terms in (24) are the ordinary Sachs-Wolfe contribution (9) discussed (a) Figure 6.…”

Section: The Spherical Space Forms and Their Vibrational Modesmentioning

confidence: 99%

“…Recent analyses concerning the suppression at low multipoles in the WMAP data can be found in [11,12,13,14,15]. As discussed before, a finite Universe is naturally obtained, if the total energy density exceeds the critical value one, i. e. Ω tot > 1.…”

Section: Introductionmentioning

confidence: 99%

CMB anisotropy of spherical spaces

Aurich

Lustig

Steiner

2005

Class. Quantum Grav.

Self Cite

128

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“…They include a cut off in the primordial power spectrum [18,19,20,21,22,23,24,25,26,27,28,29,30,31], a small universe [2,32,33,34,35] and perturbations in the dark energy [36,37,38,39,40]. The cut-off and small Universe models work by reducing the Sachs Wolfe effect in the quadrupole.…”

Section: Introductionmentioning

confidence: 99%

Low CMB quadrupole from dark energy isocurvature perturbations

2004

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We explicate the origin of the temperature quadrupole in the adiabatic dark energy model and explore the mechanism by which scale invariant isocurvature dark energy perturbations can lead to its sharp suppression. The model requires anticorrelated curvature and isocurvature fluctuations and is favored by the WMAP data at about the 95% confidence level in a flat scale invariant model. In an inflationary context, the anticorrelation may be established if the curvature fluctuations originate from a variable decay rate of the inflaton; such models however tend to overpredict gravitational waves. This isocurvature model can in the future be distinguished from alternatives involving a reduction in large scale power or modifications to the sound speed of the dark energy through the polarization and its cross correlation with the temperature. The isocurvature model retains the same polarization fluctuations as its adiabatic counterpart but reduces the correlated temperature fluctuations. We present a pedagogical discussion of dark energy fluctuations in a quintessence and k-essence context in the Appendix.

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“…Following these arguments, we will focus our attention entirely on the flat case in this work. Details on the Poincaré dodecahedral space and experimental data analysis are given in (Luminet et al 2003;Roukema 2009;Roukema et al 2004Roukema et al , 2008Caillerie et al 2007; Lew & Roukema 2008;Aurich et al 2005b), and other topologies in (Aurich & Lustig 2010;Niarchou & Jaffe 2007;Aurich et al 2006Aurich et al , 2005aCresswell et al 2006;Aurich et al 2005c;Roukema 2005;Aurich et al 2004;Riazuelo et al 2004;Gomero et al 2002a;Bond et al 2000;Mota et al 2005;Gundermann 2005).…”

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confidence: 99%

Constraints on the global topology and size of the universe from the cosmic microwave background

Aslanyan

Manohar

2012

J. Cosmol. Astropart. Phys.

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We study the possibility that the universe has compact topologies T 3 , T 2 × R 1 , or S 1 × R 2 using the seven-year WMAP data. The maximum likelihood 95% confidence intervals for the size L of the1 for the three cases, respectively, where L 0 = 14.4 Gpc is the distance to the last scattering surface. An infinite universe is compatible with the data at 4.3 σ. We find using a Bayesian analysis that the most probable universe has topology T 2 × R 1 , with L/L 0 = 1.9.

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Hyperbolic universes with a horned topology and the cosmic microwave background anisotropy

Cited by 47 publications

References 57 publications

CMB anisotropy of spherical spaces

CMB anisotropy of spherical spaces

Low CMB quadrupole from dark energy isocurvature perturbations

Constraints on the global topology and size of the universe from the cosmic microwave background

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