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We present a comprehensive examination of the three most recent versions of the L-Galaxies semi-analytic galaxy formation model, focusing on the evolution of galaxy properties across a broad stellar mass range (10⁷\: M_M₁0^12\: M_) from z=0 to z10. We compare the predictions with the latest multiband data from key astronomical surveys, including SDSS, CANDELS, and COSMOS along with HST, JWST, and ALMA. We assess the models' ability to reproduce various time-dependent galaxy scaling relations for star-forming and quenched galaxies. Key focus areas include global galaxy properties such as stellar mass functions, cosmic star formation rate density, and the evolution of the main sequence of star-forming galaxies. Additionally, we examine resolved morphological properties such as the galaxy mass-size relation, alongside core (R<1\, kpc) and effective (R<R₄) stellar-mass surface densities as a function of stellar mass. This analysis reveals that the L-Galaxies models are in qualitatively good agreement with observed global galaxy scaling relations up to z10. However, significant discrepancies exist at both low and high redshifts in accurately reproducing the number density, size, and surface density evolution of quenched galaxies. These issues are most pronounced for massive galaxies, where the simulations underpredict the abundance of quenched galaxies at z1. 5, reaching a discrepancy of a factor of 60 by z3, with sizes several times larger than observed. Therefore, we propose that the physical prescriptions governing the cessation of star formation in galaxies, such as AGN feedback and processes related to merging, require improvement to be better supported by observational data.
Vani et al. (2024) studied this question.