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We investigate the internal structure and density profiles of halos of mass$10^{10}-10^{14}~M_\odot$ in the Evolution and Assembly of Galaxies and theirEnvironment (EAGLE) simulations. These follow the formation of galaxies in a$\Lambda$CDM Universe and include a treatment of the baryon physics thought tobe relevant. The EAGLE simulations reproduce the observed present-day galaxystellar mass function, as well as many other properties of the galaxypopulation as a function of time. We find significant differences between themasses of halos in the EAGLE simulations and in simulations that follow onlythe dark matter component. Nevertheless, halos are well described by theNavarro-Frenk-White (NFW) density profile at radii larger than ~5% of thevirial radius but, closer to the centre, the presence of stars can producecuspier profiles. Central enhancements in the total mass profile are mostimportant in halos of mass $10^{12}-10^{13}M_\odot$, where the stellar fractionpeaks. Over the radial range where they are well resolved, the resulting galaxyrotation curves are in very good agreement with observational data for galaxieswith stellar mass $M_*<5\times10^{10}M_\odot$. We present an empirical fittingfunction that describes the total mass profiles and show that its parametersare strongly correlated with halo mass.

Baryon effects on the internal structure of LCDM halos in the EAGLE simulations