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

Abstract

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 their Environment (EAGLE) simulations. These follow the formation of galaxies in a $\Lambda$CDM Universe and include a treatment of the baryon physics thought to be relevant. The EAGLE simulations reproduce the observed present-day galaxy stellar mass function, as well as many other properties of the galaxy population as a function of time. We find significant differences between the masses of halos in the EAGLE simulations and in simulations that follow only the dark matter component. Nevertheless, halos are well described by the Navarro-Frenk-White (NFW) density profile at radii larger than ~5% of the virial radius but, closer to the centre, the presence of stars can produce cuspier profiles. Central enhancements in the total mass profile are most important in halos of mass $10^{12}-10^{13}{M}_{\odot }$, where the stellar fraction peaks. Over the radial range where they are well resolved, the resulting galaxy rotation curves are in very good agreement with observational data for galaxies with stellar mass $M_{\ast }<5\times 10^{10}{M}_{\odot }$. We present an empirical fitting function that describes the total mass profiles and show that its parameters are strongly correlated with halo mass.

arXiv comment21 pages, 17 figures, version accepted for publication in MNRAS

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• Milky-Way-like stars in a galaxy core 8 billion years ago revealed by gravitational lensing
• The interplay between AGN feedback and precipitation of the intracluster medium in simulations of galaxy groups and clusters
• AMICO galaxy clusters in KiDS-1000: Splashback radius from weak lensing and cluster-galaxy correlation function
• Scaling Relations in the Phase-Space Structure of Dark Matter Haloes
• Extragalactic Searches for Dark Matter Annihilation
• Cosmic Reionization On Computers: Baryonic Effects on Halo Concentrations During the Epoch of Reionization