Evolution of Galaxy Shapes from Prolate to Oblate through Compaction Events
Matteo Tomassetti, Avishai Dekel, Nir Mandelker, Daniel Ceverino,, Sharon Lapiner, Sandra Faber, Omer Kneller, Joel Primack, Tanmayi Sai

TL;DR
This study uses cosmological simulations to trace how galaxy shapes evolve from prolate, elongated forms dominated by dark matter to oblate, flattened structures aligned with gas discs, driven by compaction and feedback processes.
Contribution
It provides a detailed evolutionary pathway of galaxy shapes from high redshift to quenching, highlighting the role of compaction events and feedback in shape transformation.
Findings
High-z galaxies are prolate and triaxial, aligned with large-scale filaments.
Transition to oblate shape occurs around stellar mass of 10^9 M_sun.
Supernova feedback influences the shape evolution and core dominance.
Abstract
We study the evolution of global shapes of galaxies using cosmological simulations. The shapes refer to the components of dark matter (DM), stars and gas at the stellar half-mass radius. Most galaxies undergo a characteristic compaction event into a blue nugget at , which marks the transition from a DM-dominated central body to a self-gravitating baryonic core. We find that in the high-, DM-dominated phase, the stellar and DM systems tend to be triaxial, preferentially prolate and mutually aligned. The elongation is supported by an anisotropic velocity dispersion that originates from the assembly of the galaxy along a dominant large-scale filament. We estimate that torques by the dominant halo are capable of inducing the elongation of the stellar system and its alignment with the halo. Then, in association with the transition to self-gravity, small-pericenter orbits puff up…
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