ABSTRACT
The variations in the size of galaxies, and consequently, the formation of Low Surface Brighntess Galaxies (LSBGs) could be followed from one of two different effects: variations in the spin parameter of the halo (λ) or variations in the density of dark matter halos (McGaugh 2021). We test both scenarios by employing a simulated sample of galaxies drawn from the TNG100 run of the IllustrisTNG project. We find no significant differences in the halo concentration index between LSBGs and their High Surface Brightness (HSBGs) counterparts, with LSBGs residing in halos with higher λ than HSBGs, suggesting that variations in galaxy sizes are followed by the effect of variating λ, rather than the density of dark matter halos, specially at z~2. Extending our analysis to larger scales, we found that the relative abundance of LSBGs within groups and clusters displays a central deficit, hinting at potential destruction upon reaching these core regions. Our examination of the cosmic web reveals no significant differences in the distance to the closest large-scale structure, suggesting a limited impact of large-scale spatial distribution on mechanisms driving LSBG evolution. All together, we conclude that the halo vicinity and local environment at the scale of galaxy clusters, where mechanisms such as galaxy mergers and tidal stripping, as well as stellar and gas accretion take place, is the most likely environment that favour the emergence of LSBGs with different morphologies, mostly driven by the presence or absence of important local interaction phenomena.
Host: Dandan Xu
