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We quantify the impact of galaxy formation on dark matter halo shapes usingcosmological simulations at redshift $z=0$. The haloes are drawn from theIllustrisTNG project, a suite of magneto-hydrodynamic simulations of galaxies.We focus on haloes of mass $10^{10-14} M_\odot$ from the 50-Mpc (TNG50) and100-Mpc (TNG100) boxes, and compare them to dark matter-only (DMO) analoguesand other simulations e.g. NIHAO and Eagle. We further quantify the predictionuncertainty by varying the baryonic feedback models in a series of smaller 25Mpc $h^{-1}$ boxes. We find that: (i) galaxy formation results in rounderhaloes compared to the DMO simulations, in qualitative agreement with pasthydrodynamic models. Haloes of mass $\approx 2\times 10^{12} M_\odot$ are mostspherical, with an average minor-to-major axis ratio of $\left< s \right>\approx 0.75$ in the inner halo, an increase of 40 per cent compared to theirDMO counterparts. No significant change in halo shape is found for low-mass$10^{10} M_\odot$ haloes; (ii) stronger feedback, e.g. increasing galactic windspeed, reduces the impact of baryons; (iii) the inner halo shape correlateswith the stellar mass fraction, which can explain the dependence of halo shapeson different feedback models; (iv) the fiducial and weaker feedback models aremost consistent with observational estimates of the Milky Way halo shape. Yet,at fixed halo mass, very diverse and possibly unrealistic feedback models allpredict inner halo shapes that are closer to one another than to the DMOresults. This implies that a larger observational sample would be required tostatistically distinguish between different baryonic prescriptions due to largehalo-to-halo variation in halo shapes.

The impact of galactic feedback on the shapes of dark-matter haloes