Understanding the role of magnetic fields in star-forming regions is of fundamental importance. The interpretation of Galactic synchrotron observations is complicated by the degeneracy between the strength of the magnetic field perpendicular to the line of sight and the cosmic-ray electron (CRe) spectrum. Soon, the exceptional sensitivity of the Square Kilometre Array (SKA) will offer a unique opportunity to evaluate the magnetic field strength in molecular clouds and cloud cores through synchrotron emission observations. The most recent Voyager data, together with Galactic synchrotron emission and Alpha Magnetic Spectrometer data, constrain the flux of interstellar CRe down to 3 MeV, in particular in the energy range relevant for synchrotron emission in molecular clouds at SKA frequencies.

I will illustrate the impact that different realisations of the CRe spectrum have on interpreting the spatial variation of the spectral index and will show predictions for non-thermal emission at the smaller scales of low- and high-mass protostellar jet shocks, where the local acceleration of electrons is expected.

Brief CV of Dr. Marco Padovani:

He got his PhD in astrophysics at the Università degli Studi di Firenze and at the INAF-Osservatorio Astrofisico di Arcetri. He worked as Post Doc at the Observatorio Astronómico Nacional di Madrid, at the Institut de Ciències de l'Espai di Barcellona, at the École Normale Supérieure di Parigi, at the Laboratoire Univers et Particules di Montpellier and at the Origins Excellence Cluster in Garching. At the moment he is senior researcher at INAF-Osservatorio Astrofisico di Arcetri where he continues his research on the role played by the cosmic rays in the chemical and dynamical evolution of the star-forming regions.