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Disc galaxies commonly show asymmetric features in their morphology, such aswarps and lopsidedness. These features can provide key information regardingthe recent evolution of a given disc galaxy. In the nearby Universe, up to$\sim30$ percent of late-type galaxies display a global non-axisymmetriclopsided mass distribution. However, the origin of this perturbation is notwell understood. In this work, we study the origin of lopsided perturbations insimulated disc galaxies extracted from the TNG50 simulation of the IllustrisTNGproject. We statistically explore different excitation mechanisms for thisperturbation, such as direct satellite tidal interactions and distortions ofthe underlying dark matter distributions. We also characterize the mainphysical conditions that lead to lopsided perturbations. 50 percent of oursample galaxy have lopsided modes $m=1$ greater than $\sim 0.12$. We find astrong correlation between internal galaxy properties, such as central stellarsurface density and disc radial extension with the strength of lopsided modes.The majority of lopsided galaxies have lower central surface densities and moreextended discs than symmetric galaxies. As a result, such lopsided galaxies areless self-gravitationally cohesive, and their outer disc region is moresusceptible to different types of external perturbations. However, we do notfind strong evidence that tidal interactions with satellite galaxies are themain driving agent of lopsided modes. Lopsided galaxies tend to live inasymmetric dark matter halos with high spin, indicating strong galaxy-haloconnections in late-type lopsided galaxies.

Lopsided Galaxies in a cosmological context: a new galaxy-halo connection