Abstract
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.
Highlights
Deflection of ultra-high energy cosmic rays (UHECR), rotation measure, synchrotron radiation, and polarized dust are just a small sample of different methods of observation of the galactic magnetized interstellar medium (ISM)
In order to get an accurate description of the Synchrotron diffuse radiation (SDR) in the Galaxy, we use – for the first time in this context – 3-dimensional galactic cosmic ray electrons (GCRE) models obtained by running the DRAGON code
We have placed a constraint on the Cosmic rays (CRs) diffusive halo scale height, based on the comparison of the computed synchrotron emission intensity with radio observations
Summary
Deflection of ultra-high energy cosmic rays (UHECR), rotation measure, synchrotron radiation, and polarized dust are just a small sample of different methods of observation of the galactic magnetized interstellar medium (ISM). A parallel study of radio emission, together with CR measurements, can put better constraints on all the interstellar medium (ISM) components involved (Strong et al, 2011). The interpretation of those measurements requires a proper modelling of injection, propagation and losses in the Galaxy. We plan to accomplish the aforementioned study by running the DRAGON code in its 3-dimensional version This is well suited to model the CRE propagation, when accounting for a realistic spiral arm distribution of astrophysical sources, gas distributions, magnetic fields models and dif-.
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