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Contact. This paper is the fourth in a series dedicated to the observed parallelism of properties passing from globular clusters to early-type galaxies. To a lesser extent, it also covers galaxy clusters and groups. Aims. Here, we investigate the Ie-Re plane and the 3D-kappa space defined by Bender, Burstein and Faber, as potential diagnostic tools in studies of the past evolution of these stellar systems. In the space of the parameters characterizing a stellar system such as the luminosity, L, stellar mass, Ms, half-light (mass) radius, Re, central velocity dispersion, σc, surface brightness, Ie, and so on, the Ie-Re plane is one of possible projections that was thoroughly investigated over the years with many important results. The 3D-kappa space relies on three variables that are suitable combinations of the logarithms of the above parameters. Among others, perhaps the most important result from this new space is the discovery of the fundamental plane of early type galaxies. In this paper, we intend to explore in more detail the potential capability of the joined investigation of the Ie-Re plane and 3D-kappa space. Methods. Based on the collected literature data on the mass, half-mass (light) radius, velocity dispersion, and surface brightness in different bands for the objects under investigation, we set up the Ie-Re plane and the 3D-kappa space. We then compared the observed distributions of these objects with those predicted by simple theoretical galaxy models. Results. We explored the effects of different mass-radius relationships, star formation, infall, and mass assembling histories on the diagnostic planes under examination. We also investigated variations in the 3D-kappa space as a function of the redshift. Conclusions. We show that the distribution of the stellar systems on the various diagnostic planes can cast light on the mass-radius relation and the history of star formation in stellar systems going from globular clusters to early type galaxies.
Contact. This paper is the fourth in a series dedicated to the observed parallelism of properties passing from globular clusters to early-type galaxies. To a lesser extent, it also covers galaxy clusters and groups. Aims. Here, we investigate the Ie-Re plane and the 3D-kappa space defined by Bender, Burstein and Faber, as potential diagnostic tools in studies of the past evolution of these stellar systems. In the space of the parameters characterizing a stellar system such as the luminosity, L, stellar mass, Ms, half-light (mass) radius, Re, central velocity dispersion, σc, surface brightness, Ie, and so on, the Ie-Re plane is one of possible projections that was thoroughly investigated over the years with many important results. The 3D-kappa space relies on three variables that are suitable combinations of the logarithms of the above parameters. Among others, perhaps the most important result from this new space is the discovery of the fundamental plane of early type galaxies. In this paper, we intend to explore in more detail the potential capability of the joined investigation of the Ie-Re plane and 3D-kappa space. Methods. Based on the collected literature data on the mass, half-mass (light) radius, velocity dispersion, and surface brightness in different bands for the objects under investigation, we set up the Ie-Re plane and the 3D-kappa space. We then compared the observed distributions of these objects with those predicted by simple theoretical galaxy models. Results. We explored the effects of different mass-radius relationships, star formation, infall, and mass assembling histories on the diagnostic planes under examination. We also investigated variations in the 3D-kappa space as a function of the redshift. Conclusions. We show that the distribution of the stellar systems on the various diagnostic planes can cast light on the mass-radius relation and the history of star formation in stellar systems going from globular clusters to early type galaxies.
Using the Illustris-1 and IllustrisTNG-100 simulations, we investigate the properties of the Fundamental Plane (FP), which is the correlation between the effective radius the effective surface intensity and the central stellar velocity dispersion sigma of galaxies, at different cosmic epochs. Our aim is to study the properties of galaxies in the FP and its projections across time, adopting samples covering different intervals of mass. We would like to demonstrate that the position of a galaxy in the FP space strongly depends on its degree of evolution, which might be represented by the beta and $ L'_0$ parameters entering the law. Starting from the comparison of the basic relations among the structural parameters of artificial and real galaxies at low redshift, we obtain the fit of the FP and its coefficients at different cosmic epochs for samples of different mass limits. Then, we analyze the dependence of the galaxy position in the FP space as a function of the beta parameter and the star formation rate (SFR). We find that: 1) the coefficients of the FP change with the mass range of the galaxy sample; 2) the low luminous and less massive galaxies do not share the same FP of the bright massive galaxies; 3) the scatter around the fitted FP is quite small at any epoch and increases when the mass interval increases; 4) the distribution of galaxies in the FP space strongly depends on the beta values ( on the degree of virialization and the star formation rate). The FP is a complex surface that is well approximated by a plane only when galaxies share similar masses and condition of virialization.
We present a comprehensive examination of the three latest 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⊙ ≲ M⋆ ≲ 1012 M⊙) from z = 0 to z ≃ 10. This study is the first to compare predictions of L-Galaxies with high-redshift observations well outside the original calibration regime, utilising multiband data from surveys such as SDSS, CANDELS, COSMOS, 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 < Re) 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 scaling relations up to z ≃ 10. 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 central galaxies, where the simulations underpredict the abundance of quenched systems at z ≥ 1.5, reaching a discrepancy of a factor of 60 by z ≈ 3, with sizes several times larger than observed. Therefore, we propose that the physical prescriptions governing galaxy quenching, such as AGN feedback and processes related to merging, require improvement to be more consistent with observational data.
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