Magnetized completion of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>Λ</mml:mi><mml:mi>CDM</mml:mi></mml:math>paradigm

Giovannini, Massimo; Kunze, Kerstin E.

doi:10.1103/physrevd.77.061301

Cited by 60 publications

(139 citation statements)

References 26 publications

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“…Earlier work on FR of the CMB in cosmic magnetic fields has largely focused on the effect of a uniform magnetic field [20,21] and, when a stochastic magnetic field has been considered, a "thin" LSS was often assumed [22][23][24]. This approximation results in a tremendous technical simplification but it is not clear if it is suited to study the effects of a magnetic field with coherence scale smaller than the thickness of the LSS.…”

Section: Introductionmentioning

confidence: 99%

Primordial magnetism in the CMB: Exact treatment of Faraday rotation and WMAP7 bounds

Pogosian

Yadav

et al. 2011

Phys. Rev. D

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Faraday rotation induced B-modes can provide a distinctive signature of primordial magnetic fields because of their characteristic frequency dependence and because they are only weakly damped on small scales, allowing them to dominate B-modes from other sources. By numerically solving the full CMB radiative transport equations, we study the B-mode power spectrum induced by stochastic magnetic fields that have significant power on scales smaller than the thickness of the last scattering surface. Constraints on the magnetic field energy density and inertial scale are derived from WMAP 7-year data, and are stronger than the big bang nucleosynthesis (BBN) bound for a range of parameters. Observations of the CMB polarization at smaller angular scales are crucial to provide tighter constraints or a detection.

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Section: Introductionmentioning

confidence: 99%

Primordial magnetism in the CMB: Exact treatment of Faraday rotation and WMAP7 bounds

Pogosian

Yadav

et al. 2011

Phys. Rev. D

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“…The dominant mode is the magnetic vector mode which peaks at ∼ 2000-3000 (Mack et al 2002;Lewis 2004). The scalar magnetic mode is the dominant PMF contribution on large and intermediate angular scales (Giovannini 2007;Giovannini & Kunze 2008;Finelli et al 2008). The tensor contribution is always subdominant with respect to the other two and it is negligible for the purposes of this analysis.…”

Section: Constraints On a Stochastic Background Of Primordial Magnetimentioning

confidence: 99%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

5,084

163

2,253

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This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles ( > ∼ 40) are extremely well described by the standard spatiallyflat six-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be θ * = (1.04147 ± 0.00062) × 10 −2 , Ω b h 2 = 0.02205 ± 0.00028, Ω c h 2 = 0.1199 ± 0.0027, and n s = 0.9603 ± 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H 0 = (67.3 ± 1.2) km s −1 Mpc −1 , and a high value of the matter density parameter, Ω m = 0.315 ± 0.017. These values are in tension with recent direct measurements of H 0 and the magnituderedshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ΛCDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter ΛCDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r 0.002 < 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find N eff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N eff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = −1.13 +0.13 −0.10 . We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter ΛCDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. T...

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“…The scalar contribution has been the most subtle to calculate, and has only begun to be understood by several groups (Giovannini and Kunze 2008;Yamazaki et al 2008;Finelli, Paci and Paoletti 2008;Shaw and Lewis 2010). The anisotropic stress associated with the magnetic field leads in particular to the possibility of two types of scalar modes, a potentially dominant mode which arises before neutrino decoupling sourced by the magnetic anisotropic stress.…”

Section: Magnetic Fields and The Cosmic Microwave Backgroundmentioning

confidence: 99%

The First Magnetic Fields

et al. 2011

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We review current ideas on the origin of galactic and extragalactic magnetic fields. We begin by summarizing observations of magnetic fields at cosmological redshifts and on cosmological scales. These observations translate into constraints on the strength and scale magnetic fields must have during the early stages of galaxy formation in order to seed the galactic dynamo. We examine mechanisms for the generation of magnetic fields that operate prior during inflation and during subsequent phase transitions such as electroweak symmetry breaking and the quark-hadron phase transition. The implications of strong primordial magnetic fields for the reionization epoch as well as the first generation of stars is discussed in detail. The exotic, earlyUniverse mechanisms are contrasted with astrophysical processes that generate fields after recombination. For example, a Biermann-type battery can operate in a proto-

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Magnetized completion of theΛCDMparadigm

Cited by 60 publications

References 26 publications

Primordial magnetism in the CMB: Exact treatment of Faraday rotation and WMAP7 bounds

Primordial magnetism in the CMB: Exact treatment of Faraday rotation and WMAP7 bounds

Planck2013 results. XVI. Cosmological parameters

The First Magnetic Fields

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