The distribution of mass components in simulated disc galaxies

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authosrs. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedUsing 22 hydrodynamical simulated galaxies in a ΛCDM (Λcold dark matter) cosmological context we recover not only the observed baryonic Tully-Fisher relation, but also the observed 'massdiscrepancy-acceleration' relation, which reflects the distribution of the main of components the galaxies throughout their discs. This implies that the simulations, which span the range 52 < Vflat < 222 km s-1, where Vflat is the circular velocity at the flat part of the rotation curve, and match galaxy scaling relations, are able to recover the observed relations between the distributions of stars, gas and dark matter over the radial range for which we have observational rotation curve data. Furthermore, we explicitly match the observed baryonic to halo mass relation for the first time with simulatedgalaxies. We discuss our results in the context of the baryon cycle that is inherent in these simulations, and with regards to the effect of baryonic processes on the distribution of dark matter componentsISS, CB & GY thank the MINECO (Spain) for the financial support through the AYA2012-31101 grant. CB is funded through the Ramon y Cajal program of the MINECO. We thank DEISA for the generous allocation of resources from STFCs DiRAC Facility (COSMOS: Galactic Archaeology), the DEISA consortium, co-funded through EU FP6 project RI-031513 and the FP7 project RI-222919 (through the DEISA Extreme Computing Initiative), the PRACE-2IP Project (FP7 RI-283493)