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We use the NIHAO (Numerical Investigation of Hundred Astrophysical Objects)cosmological simulations to study the effects of galaxy formation on keyproperties of dark matter (DM) haloes. NIHAO consists of $\simeq 90$high-resolution SPH simulations that include (metal-line) cooling, starformation, and feedback from massive stars and SuperNovae, and cover a widestellar and halo mass range: $10^6 < M_* / M_{\odot} < 10^{11}$ ( $10^{9.5} <M_{\rm halo} / M_{\odot} < 10^{12.5}$). When compared to DM-only simulations,the NIHAO haloes have similar shapes at the virial radius, R_{\rm vir}, but aresubstantially rounder inside $\simeq 0.1R_{\rm vir}$. In NIHAO simulations$c/a$ increases with halo mass and integrated star formation efficiency,reaching $\sim 0.8$ at the Milky Way mass (compared to 0.5 in DM-only),providing a plausible solution to the long-standing conflict betweenobservations and DM-only simulations. The radial profile of the phase-space $Q$parameter ($\rho/\sigma^3$) is best fit with a single power law in DM-onlysimulations, but shows a flattening within $\simeq 0.1R_{\rm vir}$ for NIHAOfor total masses $M>10^{11} M_{\odot}$. Finally, the global velocitydistribution of DM is similar in both DM-only and NIHAO simulations, but in thesolar neighborhood, NIHAO galaxies deviate substantially from Maxwellian. Thedistribution is more symmetric, roughly Gaussian, with a peak that shifts tohigher velocities for Milky Way mass haloes. We provide the distributionparameters which can be used for predictions for direct DM detectionexperiments. Our results underline the ability of the galaxy formationprocesses to modify the properties of dark matter haloes.

NIHAO project II: Halo shape, phase-space density and velocity distribution of dark matter in galaxy formation simulations