Synchrotron Emission in Molecular Clouds, from the Diffuse Medium to Dense Cores and Protostellar Jets

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 realizations 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:

Marco Padovani earned his PhD in Astrophysics from the University of Florence and INAF-Arcetri Astrophysical Observatory. He has conducted research at the Observatorio Astronómico Nacional in Madrid, the Institut de Ciències de l’Espai in Barcelona, the École Normale Supérieure in Paris, the Laboratoire Univers et Particules in Montpellier, and the Origins Excellence Cluster in Garching. He is currently a senior researcher at INAF-Arcetri Astrophysical Observatory, where he continues his research on the role of cosmic rays in the chemical and dynamic evolution of star-forming regions.