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Magnetic fields are of critical importance for our understanding of theorigin and long-term evolution of the Milky Way. This is due to their decisiverole in the dynamical evolution of the interstellar medium (ISM) and theirinfluence on the star-formation process. Faraday rotation measures (RM) alongmany different sightlines across the Galaxy are a primary means to infer themagnetic field topology and strength from observations. However, theinterpretation of the data has been hampered by the failure of previousattempts to explain the observations in theoretical models and to synthesize arealistic multi-scale all-sky RM map. We here utilize a cosmologicalmagnetohydrodynamic (MHD) simulation of the formation of the Milky Way, augmentit with a novel star cluster population synthesis model for a more realisticstructure of the local interstellar medium, and perform detailed polarizedradiative transfer calculations on the resulting model. This yields a faithfulfirst principles prediction of the Faraday sky as observed on Earth. Theresults reproduce the observations of the Galaxy not only on global scales, butalso on local scales of individual star-forming clouds. They also imply thatthe Local Bubble containing our Sun dominates the RM signal over large regionsof the sky. Modern cosmological MHD simulations of the Milky Way's formation,combined with a simple and plausible model for the fraction of free electronsin the ISM, explain the RM observations remarkably well, thus indicating theemergence of a firm theoretical understanding of the genesis of magnetic fieldsin our Universe across cosmic time.

A reproduction of the Milky Way's Faraday rotation measure map in galaxy simulations from global to local scales