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

Pogosian, Levon; Yadav, Amit; Ng, Yi Fung; Vachaspati, Tanmay

doi:10.1103/physrevd.84.043530

Cited by 48 publications

(23 citation statements)

References 58 publications

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“…Details on these models involving Faraday rotation can be found in Ref. [15]. For the experiments considered here, the EB estimator is the most sensitive, as will be demonstrated.…”

Section: The Cmb and Cosmic Birefringencementioning

confidence: 73%

“…For a given multipole L, the noise level sets the minimum detectable signal for that multipole. For reference we have also shown two fiducial theoretical Faraday rotation power-spectra, for a scale-invariant and causal stochastic magnetic field [15]. It is clear from the plot that for scale invariant case largest contribution to the (S/N ) comes from large-scale (low L), while for causal magnetic fields, small scales (large L) contribute the most.…”

Section: Resultsmentioning

confidence: 96%

“…Magnetic fields are prevalent in cosmic structures at high redshift [12] and it is possible that they may have generated from primordial seed fields imprinted in the early universe (see [13] for a review). It has been shown that constraining FR using the CMB polarization information is a leading diagnostic of primordial magnetic field [14,15].…”

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confidence: 99%

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Revealing cosmic rotation

2012

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Cosmological Birefringence (CB), a rotation of the polarization plane of radiation coming to us from distant astrophysical sources, may reveal parity violation in either the electromagnetic or gravitational sectors of the fundamental interactions in nature. Until only recently this phenomenon could be probed with only radio observations or observations at UV wavelengths. Recently, there is a substantial effort to constrain such non-standard models using observations of the rotation of the polarization plane of cosmic microwave background (CMB) radiation. This can be done via measurements of the B-modes of the CMB or by measuring its T B and EB correlations which vanish in the standard model. In this paper we show that EB correlations-based estimator is the best for upcoming polarization experiments. The EB based estimator surpasses other estimators because it has the smallest noise and of all the estimators is least affected by systematics. Current polarimeters are optimized for the detection of B-mode polarization from either primordial gravitational waves or by large scale structure via gravitational lensing. In the paper we also study optimization of CMB experiments for the detection of cosmological birefringence, in the presence of instrumental systematics, which by themselves are capable of producing EB correlations; potentially mimicking CB.

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“…Details on these models involving Faraday rotation can be found in Ref. [15]. For the experiments considered here, the EB estimator is the most sensitive, as will be demonstrated.…”

Section: The Cmb and Cosmic Birefringencementioning

confidence: 73%

Section: Resultsmentioning

confidence: 96%

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Revealing cosmic rotation

2012

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“…Magnetic fields give rise to scalar, vector and tensor metric perturbations as well as fluid perturbations via the Lorentz force. Constraints on large scale primordial magnetic fields have already been derived using the CMB temperature and polarization power spectra [29][30][31][32][33][34][35][36] and Faraday rotation [37][38][39]. However, the effects of a primordial magnetic field on the CMB are relatively more pronounced in its non-Gaussian correlations.…”

Section: Introductionmentioning

confidence: 99%

Primordial magnetic field limits from the CMB trispectrum: Scalar modes and Planck constraints

2014

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Cosmic magnetic fields are observed to be coherent on large scales and could have a primordial origin. NonGaussian signals in the cosmic microwave background (CMB) are generated by primordial magnetic fields as the magnetic stresses and temperature anisotropy they induce depend quadratically on the magnetic field. We compute the CMB scalar trispectrum on large angular scales, for nearly scale-invariant magnetic fields, sourced via the Sachs-Wolfe effect. The trispectra induced by magnetic energy density and by magnetic scalar anisotropic stress are found to have typical magnitudes of approximately 10 −29 and 10 −19 , respectively. The scalar anisotropic stress trispectrum is also calculated in the flat-sky approximation and yields a similar result. Observational limits on CMB non-Gaussianity from the Planck mission data allow us to set upper limits of B0 0.6 nG on the present value of the primordial cosmic magnetic field. Considering the inflationary magnetic curvature mode in the trispectrum can further tighten the magnetic field upper limit to B0 0.05 nG. These sub-nanoGauss constraints from the magnetic trispectrum are the most stringent limits so far on the strength of primordial magnetic fields, on megaparsec scales, significantly better than the limits obtained from the CMB bispectrum and the CMB power spectrum.

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“…Stringent constraints emerge from considering different aspects of the interaction of PMF with the CMB, as well as different features and scales of these cosmic fields (see for instance [45,46], and references therein). Constraints have been derived using the CMB temperature and polarization power spectra [47][48][49][50], Faraday rotation [51][52][53], cosmic birefringence, and studying its non-Gaussian correlations, considering the bispectrum [54,55] as well as the trispectrum [56]. The upper bounds that are established are between a few and a tenth of nano Gauss.…”

Section: Scenarios For the Generation Of Cosmic Magnetic Fieldsmentioning

confidence: 99%

Magnetic fields in compact stars and related phenomena

et al. 2020

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Magnetic fields appear at all scales in the Universe, spanning many orders of magnitude in their strength, and intervening in the development of many astrophysical processes. In particular, in compact objects, magnetic fields can reach huge intensities and play a fundamental role in the evolution of the star and its surroundings. In this review, the most relevant ideas about their generation mechanisms and their eects on the composition and evolution of compact stars are summarized. The review highlights the role played by anisotropic pressures, induced by the presence of strong magnetic fields, in the equation of state and in the macroscopic observables of compact objects. Anisotropies demand to solve Einstein equations beyond the sphericalsymmetry. In this regard, two models are analyzed, one using a metric in cylindrical coordinates and another one considering a metric, which allows to take into account small deformations of the objects. These results are relevant for the description of magnetized white dwarfs and hypothetical quark and Bose-Einstein condensate stars. Some related astrophysical phenomena, as pulsar kick velocities and jets associated to compact objects, are also addressed as a consequence of the presence of strong magnetic fields.

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

Cited by 48 publications

References 58 publications

Revealing cosmic rotation

Revealing cosmic rotation

Primordial magnetic field limits from the CMB trispectrum: Scalar modes and Planck constraints

Magnetic fields in compact stars and related phenomena

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