Connecting synchrotron, cosmic rays and magnetic fields in the plane of the Galaxy
Abstract
We extend previous work modelling the Galactic magnetic field in the plane using synchrotron emission in total and polarized intensity. In this work, we include a more realistic treatment of the cosmic ray electrons using the GALPROP propagation code optimized to match the existing high-energy data. This addition reduces the degeneracies in our previous analysis and when combined with an additional observed synchrotron frequency allows us to study the low-energy end of the cosmic ray electron spectrum in a way that has not previously been done. For a pure diffusion propagation, we find a low-energy injection spectrum slightly harder than generally assumed: for J(E) ∝Eα, we find α=-1.34 ± 0.12, implying a very sharp break with the spectrum above a few GeV. This then predicts a synchrotron brightness temperature spectral index, β, on the Galactic plane, that is -2.8 < β < -2.74 below a few GHz and -2.98 < β < -2.91 up to 23 GHz. We find that models including cosmic ray re-acceleration processes appear to be incompatible with the synchrotron data.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- September 2011
- DOI:
- 10.1111/j.1365-2966.2011.19114.x
- arXiv:
- arXiv:1105.5885
- Bibcode:
- 2011MNRAS.416.1152J
- Keywords:
-
- polarization;
- radiation mechanisms: general;
- cosmic rays;
- ISM: magnetic fields;
- Galaxy: structure;
- radio continuum: ISM;
- Astrophysics - Astrophysics of Galaxies
- E-Print:
- 12 pages, 10 figures. Accepted for publication in MNRAS. This research was supported by the Agence Nationale de la Recherche (ANR-08-CEXC-0002-01)