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Free keywords:
CUSP-CORE TRANSFORMATIONS; MILLENNIUMTNG PROJECT; COSMOLOGICAL
SIMULATIONS; DENSITY PROFILES; MASS; MODEL; COLD; EVOLUTION; ABUNDANCE;
FEEDBACKAstronomy & Astrophysics; methods: numerical; galaxies: evolution; galaxies: formation; galaxies:
fundamental parameters; galaxies: structure; dark matter;
Abstract:
We investigate the redshift evolution of the concentration-mass relationship of dark matter haloes in state-of-the-art cosmological hydrodynamic simulations and their dark-matter-only (DMO) counterparts. By combining the Illustris TNG suite and the novel Millennium TNG simulation, our analysis encompasses a wide range of box size (50-740 cMpc) and mass resolution (8.5x 10(4) - 3.1 x 10(7) M-circle dot per baryonic mass element). This enables us to study the impact of baryons on the concentration-mass relationship in the redshift interval 0 < z < 7 over an unprecedented halo mass range, extending from dwarf galaxies to superclusters (similar to 10(9.5)-10(15.5) M-circle dot). We find that the presence of baryons increases the steepness of the concentration-mass relationship at higher redshift, and demonstrate that this is driven by adiabatic contraction of the profile, due to gas accretion at early times, which promotes star formation in the inner regions of haloes. At lower redshift, when the effects of feedback start to become important, baryons decrease the concentration of haloes below the mass scale similar to 10(11.5) M-circle dot. Through a rigorous information criterion test, we show that broken power-law models accurately represent the redshift evolution of the concentration-mass relationship, and of the relative difference in the total mass of haloes induced by the presence of baryons. We provide the best-fitting parameters of our empirical formulae, enabling their application to models that mimic baryonic effects in DMO simulations over six decades in halo mass in the redshift range 0 < z < 7.
