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Spectral index of synchrotron emission: insights from the diffuse and magnetised interstellar medium

Padovani, Marco; Bracco, Andrea; Jelić, Vibor; Galli, Daniele; Bellomi, Elena (2021) Spectral index of synchrotron emission: insights from the diffuse and magnetised interstellar medium. Astronomy & Astrophysics, 651 . ISSN 0004-6361

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Context. The interpretation of Galactic synchrotron observations is complicated by the degeneracy between the strength of the magnetic field perpendicular to the line of sight (LOS), B⊥, and the cosmic-ray electron (CRe) spectrum. Depending on the observing frequency, an energy-independent spectral energy slope s for the CRe spectrum is usually assumed: s = −2 at frequencies below ≃400 MHz and s = −3 at higher frequencies. Aims. Motivated by the high angular and spectral resolution of current facilities such as the LOw Frequency ARray (LOFAR) and future telescopes such as the Square Kilometre Array (SKA), we aim to understand the consequences of taking into account the energy-dependent CRe spectral energy slope on the analysis of the spatial variations of the brightness temperature spectral index, β, and on the estimate of the average value of B⊥ along the LOS. Methods. We illustrate analytically and numerically the impact that different realisations of the CRe spectrum have on the interpretation of the spatial variation of β. We use two snapshots from 3D magnetohydrodynamic simulations as input for the magnetic field, with median magnetic field strength of ≃4 and ≃20 μG, to study the variation of β over a wide range of frequencies (≃0.1−10 GHz). Results. We find that the common assumption of an energy- independent s is only valid in special cases. We show that for typical magnetic field strengths of the diffuse ISM (≃2−20 μG), at frequencies of 0.1−10 GHz, the electrons that are mainly responsible for the synchrotron emission have energies in the range ≃100 MeV−50 GeV. This is the energy range where the spectral slope, s, of CRe varies to the greatest extent. We also show that the polarisation fraction can be much smaller than the maximum value of ≃70% because the orientation of B⊥ varies across the beam of the telescope and along the LOS. Finally, we present a look-up plot that can be used to estimate the average value of B⊥ along the LOS from a set of values of β measured at different frequencies, for a given CRe spectrum. Conclusions. In order to interpret the spatial variations of β observed from centimetre to metre wavelengths across the Galaxy, the energy- dependent slope of the Galactic CRe spectrum in the energy range ≃100 MeV−50 GeV must be taken into account.

Item Type: Article
Uncontrolled Keywords: cosmic rays / ISM: magnetic fields / ISM: clouds / ISM: structure ; radio continuum: ISM ; radiation mechanisms: non-thermal
Subjects: NATURAL SCIENCES > Physics
NATURAL SCIENCES > Physics > Astronomy and Astrophysics
Divisions: Division of Experimental Physics
Project titleProject leaderProject codeProject type
Razumijevanje zračenja na niskim radio frekvencijama: ususret novoj generaciji radio teleskopaJelić, ViborIP-2018-01-2889HRZZ
Origin of Magnetic strUctureS in the ISM obscuring the Cosmic DAwnJelić, Vibor; Braco, Andrea843008EK
Depositing User: Vibor Jelić
Date Deposited: 08 Sep 2021 13:12
DOI: 10.1051/0004-6361/202140799

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