Extended Mosaic Observations with the Cosmic Background Imager

Readhead, A. C. S.; Mason, B. S.; Contaldi, C. R.; Pearson, T. J.; Bond, J. R.; Myers, S. T.; Padin, S.; Sievers, Jonathan; Cartwright, J. K.; Shepherd, M. C.; Pogosyan, D.; Prunet, S.; Altamirano, Pablo; Bustos, R.; Bronfman, L.; Casassus, S.; Holzapfel, W. L.; May, J.; Pen, Ue-Li; Torres, S.; Udomprasert, P. S.

doi:10.1086/421105

Cited by 334 publications

(320 citation statements)

References 47 publications

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“…It also provides a plausible explanation for the possible disparity between observations and theoretical fits to the CMB power-spectrum. The ACBAR [13] and CBI [14] experiments indicate continued power up to l ∼ 4000, but WMAP data predicts a rapidly declining power spectrum in the large multipole range [15]. This discrepancy is difficult to account from a returning of cosmological parameters.…”

Section: Introductionmentioning

confidence: 99%

Primordial large-scale electromagnetic fields from gravitoelectromagnetic inflation

Membiela¹,

Bellini²

2009

Physics Letters B

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We investigate the origin and evolution of primordial electric and magnetic fields in the early universe, when the expansion is governed by a cosmological constant Λ0. Using the gravitoelectromagnetic inflationary formalism with A0 = 0, we obtain the power of spectrums for large-scale magnetic fields and the inflaton field fluctuations during inflation. A very important fact is that our formalism is naturally non-conformally invariant.

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Section: Introductionmentioning

confidence: 99%

Primordial large-scale electromagnetic fields from gravitoelectromagnetic inflation

Membiela¹,

Bellini²

2009

Physics Letters B

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“…Figure 4 shows the marginalized likelihood of ξ. We obtain from the figure that 0.74 < ∼ ξ < ∼ 1.66 by WMAP data alone [21], 0.75 < ∼ ξ < ∼ 1.74 by WMAP, CBI and ACBAR data sets [22,23], at 95% confidence level.…”

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confidence: 99%

Cosmological constraints on Newton’s constant

2005

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We present cosmological constraints on deviations of Newton's constant at large scales, analyzing latest cosmic microwave background (CMB) anisotropies and primordial abundances of light elements synthesized by big bang nucleosynthesis (BBN). BBN limits the possible deviation at typical scales of BBN epoch, say at 10 8 ∼ 10 12 m, to lie between −5% and +1% of the experimental value, and CMB restricts the deviation at larger scales 10 2 ∼ 10 9 pc to be between −26% and +66% at the 2σ confidence level. The cosmological constraints are compared with the astronomical one from the evolution of isochrone of globular clusters.

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“…Using a Markov chain Monte Carlo algorithm (see, e.g., Ref. [21]), and data from SDSS [22], WMAP [23], CBI [24], VSA [25], and Type Ia supernovae [26] we find the bound shown in Fig. 1.…”

Section: Constraints From Large-scale Structure and The Cmbmentioning

confidence: 99%

How Dark is ‘Dark’? Electromagnetic Interactions in the Dark Sector

Sigurdson

Dark Matter in Astro- And Particle Physics

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Summary. We review the physical and cosmological consequences of two possible electromagnetic couplings to the dark sector: (i) a neutral lightest dark-matter particle (LDP) with nonzero electric and/or magnetic dipole moments and (ii) a charged next-to-lightest dark-matter particle (NLDP) which decays to a neutral LDP. For scenario (i) we find that a relatively light particle with mass between a few MeV and a few GeV and an electric or magnetic dipole as large as ∼ 3 × 10 −16 e cm (roughly 1.6×10 −5 µB) satisfies experimental and observational bounds. In scenario (ii), we show that charged-particles decaying in the early Universe result in a suppression of the small-scale matter power spectrum on scales that enter the horizon prior to decay. This leads to either a cutoff in the matter power spectrum, or if the charged fraction is less than unity, an effect in the power spectrum that might resemble a running (scale-dependent) spectral index in small-scale data. MotivationThe origin of the missing 'dark' matter in galaxies and clusters of galaxies has been an outstanding problem for over 70 years, since Zwicky's measurement of the masses of extragalactic systems [1]. Recent cosmological observations not only tell us how much dark matter exists but also that it must be nonbaryonic [2] -it is not one of the familiar elementary particles contained within the standard model of particle physics. Dark matter is a known unknown. We do not know what the underlying theory of dark matter is, what the detailed particle properties of it are, nor the particle spectrum of the dark sector.Promising candidates for the lightest dark-matter particle (LDP) -those that appear in minimal extensions of the standard model and are expected to have the required cosmological relic abundance -are a weakly-interacting massive particle (WIMP), such as the neutralino, the lightest mass eigenstate from the superposition of the supersymmetric partners of the U (1) and SU (2) neutral gauge bosons and of the neutral Higgs bosons [3], or the axion [4]. There is a significant theoretical literature on the properties and phenomenology of these particles, and there are ongoing experimental efforts to detect these particles.There has also been a substantial phenomenological effort toward placing model-independent limits on the possible interactions of the LDP. For instance, significant constraints have been made to dark-matter models with

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Extended Mosaic Observations with the Cosmic Background Imager

Cited by 334 publications

References 47 publications

Primordial large-scale electromagnetic fields from gravitoelectromagnetic inflation

Primordial large-scale electromagnetic fields from gravitoelectromagnetic inflation

Cosmological constraints on Newton’s constant

How Dark is ‘Dark’? Electromagnetic Interactions in the Dark Sector

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