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WMAP Polarised Filaments

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Diffuse Radio Foregrounds

Part of the book series: Springer Theses ((Springer Theses))

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Abstract

At frequencies up to a few GHz, the total radio sky brightness is dominated by the diffuse Galactic synchrotron radiation, where cosmic rays (CR) electrons and positrons spiralling

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Notes

  1. 1.

    This is calculated using \(\mathrm {FWHM_{deconv}}=\sqrt{\mathrm {FWHM_{obs}} - 1^{\circ }}\), where \(\mathrm {FWHM_{obs}}\) is the measured width of the profile. The angular resolution of the maps is 1\(^{\circ }\).

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Authors and Affiliations

  1. Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, UK

    Matías Vidal Navarro

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  1. Matías Vidal Navarro
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Correspondence to Matías Vidal Navarro .

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Vidal Navarro, M. (2016). WMAP Polarised Filaments. In: Diffuse Radio Foregrounds. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-26263-5_3

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