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ASTRA Proceedings An open-access journal for refereed proceedings in extraterrestrial research
Journal topic
Volume 2
ASTRA Proc., 2, 21-26, 2015
https://doi.org/10.5194/ap-2-21-2015
© Author(s) 2015. This work is distributed under
the Creative Commons Attribution 3.0 License.
ASTRA Proc., 2, 21-26, 2015
https://doi.org/10.5194/ap-2-21-2015
© Author(s) 2015. This work is distributed under
the Creative Commons Attribution 3.0 License.

  22 Sep 2015

22 Sep 2015

Diffuse synchrotron emission from galactic cosmic ray electrons

G. Di Bernardo1, D. Grasso2, C. Evoli3, and D. Gaggero4,5 G. Di Bernardo et al.
  • 1MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
  • 2Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, Largo B. Pontecorvo, 56127 Pisa, Italy
  • 3II. Institut für Theoretische Physik, Universität Hamburg, Luruper Chaussee 149, 22761 Hamburg, Germany
  • 4SISSA, Via Bonomea 265, 34136 Trieste, Italy
  • 5INFN, sezione di Trieste, via Valerio 2, 34127 Trieste, Italy

Abstract. Synchrotron diffuse radiation (SDR) emission is one of the major Galactic components, in the 100 MHz up to 100 GHz frequency range. Its spectrum and sky map provide valuable measure of the galactic cosmic ray electrons (GCRE) in the relevant energy range, as well as of the strength and structure of the Galactic magnetic fields (GMF), both regular and random ones. This emission is an astrophysical sky foreground for the study of the Cosmic Microwave Background (CMB), and the extragalactic microwave measurements, and it needs to be modelled as better as possible. In this regard, in order to get an accurate description of the SDR in the Galaxy, we use – for the first time in this context – 3-dimensional GCRE models obtained by running the DRAGON code. This allows us to account for a realistic spiral arm pattern of the source distribution, demanded to get a self-consistent treatment of all relevant energy losses influencing the final synchrotron spectrum.

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Magnetic fields permeate the interstellar medium (ISM), extending far beyond the Galactic disc. The non-thermal phenomena, like e.g. the Galactic radio emission is doubtless a viable method of observation to clearly delineate the magnetic structure of our Galaxy. In this regard, the aim addressed in this contribution is to simulate the polarized Galactic synchrotron emission, due to the diffuse radiation by charged relativistic particles, at all relevant frequencies, 10 MHz up to 100 GHz.
Magnetic fields permeate the interstellar medium (ISM), extending far beyond the Galactic disc....
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