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Integral field spectroscopy has allowed astronomers to probe the local variations of properties within galaxies revealing the physical processes governing their local and global star formation activity. Large galaxy surveys (e.g., MaNGA), as well as simulations (e.g., IllustrisTNG), have revealed radial trends in star formation with respect to the star-forming main sequence (SFMS). However, unifying observational and theoretical results is challenging. Utilizing adaptive optics with MUSE, the MAGPI survey allows us to extend results in the local universe, to a crucial time of 4 Gyr ago (z ~ 0.3) when simulations predict the greatest diversity in evolutionary pathways for central and satellite galaxies. Furthermore, MAGPI aims to bridge the gap between observations and simulations by creating MUSE-matched mock data cubes from a suite of simulations as a means of direct comparison. In this end-of-thesis talk, I will discuss the physical processes governing the star formation activity of galaxies at z ~ 0.3 as seen with MAGPI and three cosmological simulations - EAGLE, Magneticum, and IllustrisTNG. |
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