The characterization of primeval galaxies is a key question of modern astrophysics. With the advent of JWST and the ongoing work of ALMA, for the first time we can fully probe the spectrum of the first galaxies from the UltraViolet/optical to the Far Infrared, to have a broad view of the various phases constituting the Interstellar Medium of galaxies in the Epoch of Reionization (EoR). To exhaustively interpret such exquisite observations, it is necessary to compare with likewise refined models. In this talk, I will present results from a suite of high-resolution (30 pc and 10^4 solar masses) cosmological zoom-in simulations of galaxies in the EoR that are able to accurately follow their radiative, hydrodynamical, and chemical evolution. Combining such simulations with state-of-the-art line and continuum emission models allows us to fairly compare with the exciting results from ALMA and JWST, e.g. to study the presence of quenched galaxies already at z~7.4 and to explain the emergence of dynamically cold disks at z>5. I will conclude by pinpointing the possible limitations of current simulations, i.e. showing which physical ingredients are now missing and might explain the over-abundance of z>10 galaxies inferred by the luminosity functions: such analysis is critical in order to improve our models and thus further our physical understanding.
Mauro D'Onofrio
