CMB constraints on a stochastic background of primordial magnetic fields

Paoletti, D.; Finelli⋆, F.

doi:10.1103/physrevd.83.123533

Cited by 89 publications

(135 citation statements)

References 167 publications

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“…The new constraints are consistent with, and slightly tighter, than previous limits based on combining WMAP-7 data with highresolution CMB data (see e.g. Paoletti & Finelli 2011Shaw & Lewis 2012). …”

Section: Constraints On a Stochastic Background Of Primordial Magnetisupporting

confidence: 72%

“…For the computation of magnetized angular power spectra, we use the analytic approximations for the PMF energymomentum tensor components given in Paoletti & Finelli (2011). We consider here the regular mode for magnetic scalar perturbations, with the initial conditions of Paoletti et al (2009) (see Giovannini 2004 for earlier calculations) and Shaw & Lewis (2010) (which describes the singular passive mode, depending on the generation time of PMF).…”

Section: Constraints On a Stochastic Background Of Primordial Magnetimentioning

confidence: 99%

See 1 more Smart Citation

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

5,001

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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Section: Constraints On a Stochastic Background Of Primordial Magnetisupporting

confidence: 72%

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

5,001

163

2,253

View full text Add to dashboard Cite

show abstract

“…So far the strongest constraints have come from measurements of the cosmic microwave background (CMB) and big-bang nucleosynthesis [1,[4][5][6][7]. The CMB bounds are derived by considering the effects of Faraday rotation induced by the PMF on the CMB power spectra.…”

Section: Pacs Numbersmentioning

confidence: 99%

Chameleon-photon mixing in a primordial magnetic field

Schelpe

2010

Phys. Rev. D

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The existence of a sizable, O 10 −10 -10 −9 G , cosmological magnetic field in the early Universe has been postulated as a necessary step in certain formation scenarios for the large scale O(µG) magnetic fields found in galaxies and galaxy clusters. If this field exists then it may induce significant mixing between photons and axion-like particles (ALPs) in the early Universe. The resonant conversion of photons into ALPs in a primordial magnetic field has been studied elsewhere by Mirizzi, Redondo and Sigl (2009). Here we consider the non-resonant mixing between photons and scalar ALPs with masses much less than the plasma frequency along the path, with specific reference to the chameleon scalar field model. The mixing would alter the intensity and polarization state of the cosmic microwave background (CMB) radiation. We find that the average modification to the CMB polarization modes is negligible. However the average modification to the CMB intensity spectrum is more significant and we compare this to high precision measurements of the CMB monopole made by the far infrared absolute spectrophotometer (FIRAS) on board the COBE satellite. The resulting 95% confidence limit on the scalar-photon conversion probability in the primordial field (at 100 GHz) isP γ↔φ < 2.6 × 10 −2 . This corresponds to a degenerate constraint on the photonscalar coupling strength, g eff , and the magnitude of the primordial magnetic field. Taking the upper bound on the strength of the primordial magnetic field derived from the CMB power spectra, B λ ≤ 5.0 × 10 −9 G, this would imply an upper bound on the photon-scalar coupling strength in the range g eff 7.14 × 10 −13 GeV −1 to g eff 9.20 × 10 −14 GeV −1 , depending on the power spectrum of the primordial magnetic field.

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“…PMF can naturally arise in the early Universe thanks to mechanisms related to inflation or phase transitions and may represent the progenitors of the fields we observe on large scale structures. PMF have several impact on CMB anisotropies [19,18] …”

Section: Inflationmentioning

confidence: 99%

Planck 2015 cosmological results

Perdereau¹

2016

AIP Conference Proceedings

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CMB constraints on a stochastic background of primordial magnetic fields

Cited by 89 publications

References 167 publications

Planck2013 results. XVI. Cosmological parameters

Planck2013 results. XVI. Cosmological parameters

Chameleon-photon mixing in a primordial magnetic field

Planck 2015 cosmological results

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