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In Xie et al. 2024 we present predictions from the latest version of our model for the quenched fractions up to z~7, and study the physical mechanism responsible for quenching the first galaxies. We find that, independently of galaxy stellar mass, the dominant quenching mechanism at high redshift is feedback from central massive black holes in the form of quasar winds. This is triggered by mergers in more massive galaxies, and by disk instabilities in low-mass galaxies. Environmental quenching becomes (increasingly) important at lower redshift. 

In De Lucia et al. 2024 we present the latest version of our GAEA model, now merging our updated treatment of AGN feedback, including an explicit treatment of quasar winds, with our improved treatment of satellite evolution and explicit treatment of the partition of cold gas in its molecular and atomic components. This latest version of our model predicts specific star formation rat distributions that are in remarkable agreement with data in the local Universe, and quenched fractions that are in very nice agreement with data up to z~3-4.  Our new model predicts number densities of massive quiescent galaxies at z>3 that are the largest among recently published models, albeit still on the low side when compared with lates measurements based on JWST data. We shown that the expected cosmic variance is large, and that it can easily accomodate some of these recent measurements. 

In De Lucia et al. 2023 we present an end-to-end description of the formation process of globular clusters (GCs) which includes a treatment for their formation and dynamical evolution with our GAEA model. Our reference model reproduces well the observed correlation between the total mass in GCs and the parent halo mass. A deviation from linearity is predicted at low halo masses, which is driven by a strong dependence on morphological type. An environmental dependence of GC radii is required to reproduce the observed mass distribution of GCs in our Galaxy at the low-mass end. The metallicity distribution measured for Galactic GCs is well reproduced by our model, even though it predicts systematically younger GCs than observed. We argue that this adds further evidence for an anomalously early formation of the stars in our Galaxy.

In Zakharova et al. 2023 we apply DisPerSE to predictions from GAEA to investigate the correspondence between filaments extracted using the distribution of dark matter particles and galaxies, within the same cosmological volume. We focus in particular on filaments around massive clusters (Virgo and Coma-like). We find that filaments extracted using different tracers are broadly consistent but never coincide perfectly.   

Lustig et al. 2022 study the stellar population and structural properties of massive log(𝑀★/𝑀⊙) > 11 galaxies at 𝑧 ≈ 2.7 in the Magneticum and IllustrisTNG hydrodynamical simulations and in the GAEA semi-analytic model. No scarcity of quiescent galaxies is found at this high redshift, with GAEA reproducing quite well the fraction of observed quiescent galaxies.