Abstract

While simulations can model galaxy formation and evolution at high resolutions, reproducing observations remains challenging. Significant work has been done towards creating synthetic data cubes from simulations, mimicking the data we obtain from integral field spectrographs. This aligns with a key objective of the MAGPI survey, an ESO MUSE Large Program designed to bridge the gap between observations and simulations at lookback times of 3 – 4 Gyrs (z = 0.3). Combining adaptive optics with MUSE has resulted in spatially resolved maps of stellar and ionised gas for hundreds of galaxies beyond z = 0, which has allowed us to capture radial trends of star formation in galaxies from above to below the star-forming main sequence (SFMS). This investigation reveals that starburst galaxies are shown to evolve from uniformly to centrally enhanced star formation (SF) across cosmic time with the most significant evolution at late times. Using mock observations from EAGLE , IllustrisTNG, and Magneticum simulations, we now investigate the internal and external mechanisms shaping the radial trends of MAGPI galaxies. A good agreement between observations and simulations is only found for galaxies far below the SFMS , where we capture evidence for inside-out quenching. The simulations broadly agree between 1 – 4.5 Re but show varying central suppression within R ~ 1.5 Re for galaxies on and below the SFMS , attributable to different AGN feedback prescriptions. Central galaxies are subject to internal and external mechanisms, showing increased SF suppression in the centre with increasing halo mass, indicating AGN feedback. Satellites display increasing suppression in the outskirts as halo mass increases, indicative of environmental processes. These results demonstrate the power of spatially resolved studies of galaxies; while global properties align, radial profiles reveal discrepancies between observations and simulations and their underlying physics.