Cataldi, P.Pedrosa, S.E.Tissera, P.B.Artale, M.C.Padilla, N.D.Dominguez-Tenreiro, R.Bignone, L.Gonzalez, R.Pellizza, L.J.2023-11-222023-11-222023-08-01Monthly Notices of the Royal Astronomical Society, Volume 523, Issue 2, Pages 1919 - 1932, 1 August 202300358711https://repositorio.unab.cl/xmlui/handle/ria/54033INDEXACIÓN: SCOPUS.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. © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.encosmology: dark mattercosmology: theorygalaxies: clusters: generalgalaxies: haloesmethods: numericalArtículo10.1093/mnras/stad1601