Planck 2015 results: XIX. Constraints on primordial magnetic fields

We predict 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, related to their contribution to cosmological perturbations; the effect on CMB polarization induced by Faraday rotation; 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 derived from different combinations of Planck data products, depending on the specific effect that is analysed. Overall, Planck data constrain the amplitude of PMFs to less than a few nanogauss, with different bounds depending on the considered model. In particular, individual limits coming from the analysis of the CMB angular power spectra, using the Planck likelihood, are B1Mpc < 4:4 nG (where B1Mpc is the comoving field amplitude at a scale of 1 Mpc) at 95 % confidence level, assuming zero helicity, and B1Mpc < 5:6 nG when we consider a maximally helical field. For nearly scaleinvariant PMFs we obtain B1Mpc < 2:1 nG and B1Mpc < 0:7 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 B1Mpc < 2:8 nG. A search for preferred directions in the magnetically-induced passive bispectrum yields B1Mpc < 4:5 nG, whereas the the compensated-scalar bispectrum gives B1Mpc < 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 B1Mpc < 1380 nG. In our final analysis, we consider the harmonic-space correlations produced by Alfv´ en 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.

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Rachen | A. Zacchei | D. Maino | L. Perotto | M. Douspis | C. Rosset | A. Benoit | F.-X. D'esert | J. F. Mac'ias-P'erez | J. Delabrouille | S. Matarrese | L. Valenziano | A. Benoit-L'evy | A. Zonca | T. S. Kisner | M. Shiraishi | E. Calabrese | M. Arnaud | M. Tomasi | A. H. Jaffe | O. Forni | G. Patanchon | F. Levrier | H. C. Chiang | S. Donzelli | F. Couchot | M. Juvela | J. P. Leahy | P. M. Lubin | A. Gregorio | R. B. Barreiro | B. Rusholme | D. Scott | A. Ducout | C. Renault | D. Munshi | R. Keskitalo | E. Franceschi | A. Hornstrup | P. McGehee | L. Danese | C. Baccigalupi | L. Mendes | H. U. Norgaard-Nielsen | J. M. Diego | G. Hurier | M. Lattanzi | M. Kunz | H. Kurki-Suonio | V. Pettorino | L. Popa | A. Renzi | J. Tuovinen | F. Pasian | L. Valenziano | H. Kurki-Suonio | P. Lilje | N. Aghanim | C. Baccigalupi | K. Benabed | M. Kunz | G. Morgante | M. Douspis | M. Frailis | A. Zacchei | S. Colombi | J. Lesgourgues | A. Melchiorri | V. Pettorino | P. McGehee | J. Rubino-Mart'in | O. 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