Browsing by Author "Artale, M. C."

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    Baryons shaping dark matter haloes
    (2021) Cataldi, P.; Pedrosa, S. E.; Tissera, P. B.; Artale, M. C.
    In this work, we aim at investigating the effects of baryons on the dark matter (DM) haloes structure, focusing on the correlation between the presence and importance of stellar discs and the halo shapes. We study the properties of a subsample of DM haloes from Fenix and eagle cosmological simulations. We inspect the central regions of haloes in the mass range at z = 0, comparing the hydrodynamic runs and their dark matter only (DMo) counterparts. Our results indicate that baryons have a significant impact on the shape of the inner halo, mainly within similar to 20per cent of the virial radius. We find haloes to be more spherical when hosting baryons. While the impact of baryons depends on the mass of the haloes, we also find a trend with morphology which suggests that the way baryons are assembled is also relevant in agreement with previous works. Our findings also indicate that disc galaxies preferentially form in haloes whose DMo counterparts were originally more spherical and with stronger velocity anisotropy. The presence of baryons alter the orbital structure of the DM particles of the haloes, which show a decrease in their velocity anisotropy, towards more tangentially biased orbits. This relative decrease is weaker in the case of disc-dominated galaxies. Our results point out to a cosmological connection between the final morphology of galaxies and the intrinsic properties of their DM haloes, which gets reinforce by the growth of the discs.
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    Redshift evolution of the dark matter haloes shapes
    (2023) Cataldi, P.; Pedrosa, S. E.; Tissera, P. B.; Artale, M. C.; Padilla, N. D.; Dominguez-Tenreiro, R.; Bignone, L.; Gonzalez, R.; Pellizza, L. J.
    In this work, we aim at investigating the morphology evolution of Milky Way mass-like dark matter haloes selected from the cielo and IllustrisTNG projects. The connection between halo shapes and their environment has been studied in previous works at z = 0 but their connection remains yet to be fully understood. We focus on the evolution across cosmic time of the halo shapes and the relation with the infalling material, using hydrodynamical simulations. Our findings show that haloes tend to be more triaxial at earlier times as a consequence of stronger accretion in the direction of the filaments. As the haloes evolve towards a dominant isotropic accretion mode and relaxation, their shape at 20 per cent of the virial radius becomes more spherical. In agreement with previous results, baryons have an important effect within the inner regions of the haloes, driving them from triaxial to rounder shapes. We also find a correlation between the strength of the quadrupole infalling mode and the degree of ellipticity of the haloes: as the filament strength decreases steadily with redshift, the haloes became more spherical and less elliptical.
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    The manifestation of secondary bias on the galaxy population from IllustrisTNG300
    (2020) Montero Dorta, A. D.; Artale, M. C.; Abramo, L. R.; Tucci, B.; Padilla, Nelson; Sato Polito, G.; Lacerna Zambrano, Iván Andrés; Rodríguez, F.; Angulo, R. E.