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Abstract The measurements of morphological indicators of galaxies are often influenced by a series of observational effects. In this study, we utilize a sample of 832 TNG50 simulated galaxies with log( M * / M ⊙ )> 9 at 0.5 1 μ m. The morphological indicators of star-forming galaxies (SFGs) and quiescent galaxies (QGs) are significantly different. The morphologies of QGs exhibit a higher sensitivity to rest-frame wavelength than SFGs. After analyzing the evolution of morphological indicators in the rest-frame V band (0.5–0.7 μ m) and rest-frame J band (1.1–1.4 μ m), we find that the morphologies of QGs evolve substantially with both redshift and stellar mass. For SFGs, the C , Gini , and M 20 show a rapid evolution with stellar mass at log( M * / M ⊙ ) ≥ 10.5, while the A O , D O , and A evolve with both redshift and stellar mass. Our comparison shows that TNG50 simulations effectively reproduce the morphological indicators we measured from JWST observations when the impact of dust attenuation is considered.
Ren et al. (Fri,) studied this question.