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Faraday rotation in CMB maps

Published online by Cambridge University Press:  12 October 2016

Beatriz Ruiz-Granados ,
Eduardo Battaner  and
Estrella Florido
Beatriz Ruiz-Granados
Affiliation:
Departamento de Fsica Terica y del Cosmos, Universidad de Granada, Spain Instituto de Fsica Terica y Computacional Carlos I, Granada, Spain email: [email protected], [email protected], [email protected]
Eduardo Battaner
Affiliation:
Departamento de Fsica Terica y del Cosmos, Universidad de Granada, Spain Instituto de Fsica Terica y Computacional Carlos I, Granada, Spain email: [email protected], [email protected], [email protected]
Estrella Florido
Affiliation:
Departamento de Fsica Terica y del Cosmos, Universidad de Granada, Spain Instituto de Fsica Terica y Computacional Carlos I, Granada, Spain email: [email protected], [email protected], [email protected]
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Abstract

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WMAP CMB polarization maps have been used to detect a low signal of Faraday Rotation (FR). If this detection is not interpreted as simple noise, it could be produced:

at the last scattering surface (LSS) (z=1100), being primordial,

at Reionization (z=10),

in the Milky Way.

The second interpretation is favoured here. In this case magnetic fields at Reionization with peak values of the order of 10-8 G should produce this observational FR.

Keywords

cosmic microwave backgroundpolarizationmagnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 626 - 627
Copyright
Copyright © International Astronomical Union 2016 

References

Hinshaw, G., Larson, D., Komatsu, E., et al. 2013, ApJS 208 19; Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2013, arXiv:1303.5076 Google Scholar