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

Trivedi, Pranjal; Subramanian, Kandaswamy; Seshadri, T. R.

doi:10.1103/physrevd.89.043523

Cited by 53 publications

(54 citation statements)

References 94 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is because magnetic forcing (as described by the magnetic energy momentum tensor) is quadratic in the magnetic fields and therefore the resulting fluctuations are non-Gaussian even for Gaussian fields 10 (Brown & Crittenden 2005). There are already published theoretical studies of the passive-mode bispectra (Trivedi et al 2010;Shiraishi et al 2011Shiraishi et al , 2012Shiraishi 2013), as well as studies of the compensated-mode bispectra (Seshadri & Subramanian 2009;Caprini et al 2009;Cai et al 2010;Shiraishi et al 2010;Kahniashvili & Lavrelashvili 2010) and of trispectra (Trivedi et al 2012(Trivedi et al , 2014. This illustrates that it is possible to use CMB non-Gaussianities to constrain the PMF amplitude for different generation mechanisms.…”

Section: Magnetically-induced Non-gaussianitiesmentioning

confidence: 96%

Planck2015 results

Ade

Aghanim

Arnaud

et al. 2016

A&A

302

107

View full text Add to dashboard Cite

We compute and investigate four types of imprint of a stochastic background of primordial magnetic fields (PMFs) on the cosmic microwave background (CMB) anisotropies: the impact of PMFs on the CMB temperature and polarization spectra, which is related to their contribution to cosmological perturbations; the effect on CMB polarization induced by Faraday rotation; the impact of PMFs on the ionization history; magnetically-induced non-Gaussianities and related non-zero bispectra; and the magnetically-induced breaking of statistical isotropy. We present constraints on the amplitude of PMFs that are derived from different Planck data products, depending on the specific effect that is being analysed. Overall, Planck data constrain the amplitude of PMFs to less than a few nanoGauss, with different bounds that depend on the considered model. In particular, individual limits coming from the analysis of the CMB angular power spectra, using the Planck likelihood, are B 1 Mpc < 4.4 nG (where B 1 Mpc is the comoving field amplitude at a scale of 1 Mpc) at 95% confidence level, assuming zero helicity. By considering the Planck likelihood, based only on parity-even angular power spectra, we obtain B 1 Mpc < 5.6 nG for a maximally helical field. For nearly scale-invariant PMFs we obtain B 1 Mpc < 2.0 nG and B 1 Mpc < 0.9 nG if the impact of PMFs on the ionization history of the Universe is included in the analysis. From the analysis of magnetically-induced non-Gaussianity, we obtain three different values, corresponding to three applied methods, all below 5 nG. The constraint from the magnetically-induced passive-tensor bispectrum is B 1 Mpc < 2.8 nG. A search for preferred directions in the magneticallyinduced passive bispectrum yields B 1 Mpc < 4.5 nG, whereas the compensated-scalar bispectrum gives B 1 Mpc < 3 nG. The analysis of the Faraday rotation of CMB polarization by PMFs uses the Planck power spectra in EE and BB at 70 GHz and gives B 1 Mpc < 1380 nG. In our final analysis, we consider the harmonic-space correlations produced by Alfvén waves, finding no significant evidence for the presence of these waves. Together, these results comprise a comprehensive set of constraints on possible PMFs with Planck data.

show abstract

Section: Magnetically-induced Non-gaussianitiesmentioning

confidence: 96%

Planck2015 results

Ade

Aghanim

Arnaud

et al. 2016

A&A

302

107

View full text Add to dashboard Cite

show abstract

“…They have a strength of the order of few µG at a coherent length scale of a few tens of kpc for clusters of galaxies and a few kpc for galaxies [21,22]. The strength of these magnetic fields is constrained from the structure formation, big bang nucleosynthesis (BBN) and temperature anisotropies and polarization of cosmic microwave background (CMB) [23,24]. Anisotropy generated by homogeneous magnetic fields, whose maximal amplitude measured by PLANCK today is B 0 ≤ 4.4 nG at a comoving scale of 1 Mpc [25].…”

Section: Introductionmentioning

confidence: 99%

Baryon-Dark matter interaction in presence of magnetic fields in light of EDGES signal

et al. 2020

View full text Add to dashboard Cite

The Experiment to Detect the Global Epoch of reionization Signature (EDGES) collaboration has reported an excess absorption dip in the 21 cm signal during cosmic dawn era. The stronger than expected 21 absorption signal indicates that gas was much cooler than the standard cosmological prediction. The observed 21-cm signal can be explained by decreasing the gas temperature via baryon-DM interaction. In this work, we study the temperature evolution of the gas and Dark Matter (DM) in the presence of magnetic fields. The magnetic heating via ambipolar diffusion and the turbulent decay increases both the gas and DM temperature at low redshift and this heating is more in the favour of baryons compared to DM. In the presence of strong magnetic field, a large baryon-DM interaction cross section is required to balance magnetic heating to explain the EDGES signal as compared to weak magnetic field. We also study the brightness temperature during the cosmic dawn era and put constraint on the strength of the magnetic field for a particular mass and baryon-DM cross section.

show abstract

“…Recent results from the PLANCK collaboration have put an upper limit on the strength of a primordial field at the surface of the last scattering of the order of B0 0.55 − 5.6nG (Ade et al 2015). The additional analysis of non-Gaussianity in the Cosmic Microwave Background have further suggested slightly lower upper limits, in the range B0 0.05 − 0.6nG (Trivedi et al 2014). These limits translate into a slightly lower limit on the present-day magnetisation of voids in absence of other sources of magnetisation, B void ≈ B0(ρv/ ρ ) 2/3 (where ρv is the gas density in voids and ρ is the average gas density of the Universe).…”

Section: Introductionmentioning

confidence: 99%

Propagation of ultrahigh energy cosmic rays in extragalactic magnetic fields: a view from cosmological simulations

Hackstein¹,

Vazza²,

Brüggen³

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We use the CRPropa code to simulate the propagation of ultra high energy cosmic rays (with energy 10 18 eV and pure proton composition) through extragalactic magnetic fields that have been simulated with the cosmological ENZO code. We test both primordial and astrophysical magnetogenesis scenarios in order to investigate the impact of different magnetic field strengths in clusters, filaments and voids on the deflection of cosmic rays propagating across cosmological distances. We also study the effect of different source distributions of cosmic rays around simulated Milky-Way like observers. Our analysis shows that the arrival spectra and anisotropy of events are rather insensitive to the distribution of extragalactic magnetic fields, while they are more affected by the clustering of sources within a ∼ 50 Mpc distance to observers. Finally, we find that in order to reproduce the observed degree of isotropy of cosmic rays at ∼ EeV energies, the average magnetic fields in cosmic voids must be ∼ 0.1 nG, providing limits on the strength of primordial seed fields.

show abstract

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

Cited by 53 publications

References 94 publications

Planck2015 results

Planck2015 results

Baryon-Dark matter interaction in presence of magnetic fields in light of EDGES signal

Propagation of ultrahigh energy cosmic rays in extragalactic magnetic fields: a view from cosmological simulations

Contact Info

Product

Resources

About