Erratum: Ellipsoidal Universe Can Solve the Cosmic Microwave Background Quadrupole Problem [Phys. Rev. Lett.<b>97</b>, 131302 (2006)]

Campanelli, Leonardo; Cea, Paolo; Tedesco, Luigi

doi:10.1103/physrevlett.97.209903

Cited by 117 publications

(208 citation statements)

References 0 publications

Supporting

Mentioning

200

Contrasting

Unclassified

Order By: Relevance

“…The robustness of these anomalies have gained strength after the release of the Planck data [4,5], since several of the initial WMAP anomalies have survived the completely different pipeline analysis of the Planck collaboration [25][26][27][28] (see [29] for a comprehensive review). Since their initial report, several models in which isotropy is explicitly violated have been offered as possible mechanism for the reported anomalies [30][31][32][33]. It is thus interesting to ask what are the generic consequences of anisotropic models to the spectrum of CMB at large scales.…”

Section: Relation To Cmb Statistical Anomaliesmentioning

confidence: 99%

Isotropization of the universe during inflation

Pereira

Pitrou

2015

Comptes Rendus. Physique

View full text Add to dashboard Cite

A primordial inflationary phase allows one to erase any possible anisotropic expansion thanks to the cosmic no-hair theorem. If there is no global anisotropic stress, then the anisotropic expansion rate tends to decrease. What are the observational consequences of a possible early anisotropic phase? We first review the dynamics of anisotropic universes and report analytic approximations. We then discuss the structure of dynamical equations for perturbations and the statistical properties of observables, as well as the implication of a primordial anisotropy on the quantization of these perturbations during inflation. Finally we briefly review models based on primordial vector field which evade the cosmic no-hair theorem.PACS numbers: 98.80.-k, 98.80.Cq

show abstract

Section: Relation To Cmb Statistical Anomaliesmentioning

confidence: 99%

Isotropization of the universe during inflation

Pereira

Pitrou

2015

Comptes Rendus. Physique

View full text Add to dashboard Cite

show abstract

“…That way, the only modified component of the total quadrupole, in that frame, is a 20 . However, in a general frame with the velocities along the direction (θ, φ) the total quadrupole becomes [13]:…”

Section: Effects On the Quadrupolementioning

confidence: 99%

Large-scale cosmic flows and moving dark energy

Jiménez

Maroto

2009

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Abstract. Large-scale matter bulk flows with respect to the cosmic microwave background have very recently been detected on scales < ∼ 100h −1 Mpc andMpc by using two different techniques showing an excellent agreement in the motion direction. However, the unexpectedly large measured amplitudes are difficult to understand within the context of standard ΛCDM cosmology. In this work we show that the existence of such a flow could be signaling the presence of moving dark energy at the time when photons decoupled from matter. We also comment on the relation between the direction of the CMB dipole and the preferred axis observed in the quadrupole in this scenario.Large-scale cosmic flows and moving dark energy 2

show abstract

“…As we already remarked, the angular power in quadrupole, C 2 , is less than expected. To measure C 2 , we expand the temperature anisotropy in terms of spherical harmonics (Campanelli et al 2006;Copi et al 2004)…”

Section: Large-angle Anomalies Of Cmbmentioning

confidence: 99%

“…Although the WMAP data are regarded as a dramatic confirmation of standard inflationary cosmology (Vale 2005;de Oliveira-Costa & Tegmark 2006;Gaztañaga et al 2003;Gordon et al 2005), some anomalous features have emerged (Inoue & Silk 2006;Campanelli et al 2006;Dominik et al 2004). Firstly, the amplitude of the quadrupole is substantially less than the expectation from the best-fit ΛCDM standard model (Abramo et al 2006;de Oliveira-Costa et al 2004;Efstathiou 2004), which was found by COBE a decade ago (Bennett et al 1996) and confirmed by WMAP (Spergel et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Modeling the WMAP large-angle anomalies as an effect of a local density inhomogeneity

Guo

2010

Res. Astron. Astrophys.

View full text Add to dashboard Cite

We investigate large-angle scale temperature anisotropy in the Cosmic Microwave Background (CMB) with the Wilkinson Microwave Anisotropy Probe (WMAP) data and model the large-angle anomalies as the effect of the CMB quadrupole anisotropies caused by the local density inhomogeneities. The quadrupole caused by the local density inhomogeneities is different from the special relativity kinematic quadrupole. If the observer inhabits a strong inhomogeneous region, the local quadrupole should not be neglected. We calculate such local quadrupole under the assumption that there is a huge density fluctuation field in direction (284• , 74• ), where the density fluctuation is 10 −3 , and its center is ∼ 112h −1 Mpc away from us. After removing such mock signals from WMAP data, the power in quadrupole, C 2 , increases from the range (200 ∼ 260µK2 ) to ∼ 1000µK 2 . The quantity S, which is used to estimate the alignment between the quadrupole and the octopole, decreases from (0.7 ∼ 0.74) to (0.31 ∼ 0.37), while the model predict that C 2 = 1071.5µK 2 , S = 0.412. So our local density inhomogeneity model can, in part, explain the WMAP low-ℓ anomalies.

show abstract

Erratum: Ellipsoidal Universe Can Solve the Cosmic Microwave Background Quadrupole Problem [Phys. Rev. Lett.97, 131302 (2006)]

Cited by 117 publications

References 0 publications

Isotropization of the universe during inflation

Isotropization of the universe during inflation

Large-scale cosmic flows and moving dark energy

Modeling the WMAP large-angle anomalies as an effect of a local density inhomogeneity

Contact Info

Product

Resources

About