Size matters: abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE

ABADI MARIO GABRIEL; CRAIN ROB; JOOP SCHAYE; NAVARRO JULIO F; BOWER RICHARD; MATTHIEU SCHALLER; FERRERO ISMAEL; SALES LAURA V; FRENK CARLOS; TOM THEUNS

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Lugar: Londres; Año: 2017 vol. 464 p. 4736 - 4746

0035-8711

The Tully-Fisher relation (TFR) links the stellar mass of a disk galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the massvelocity scaling (M ∝ V3) of dark matter halos, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxyhalo mass relation to be non-monotonic and rapidy evolving. We study the TFR ofluminous spirals and its relation to AM using the EAGLE set of ΛCDM cosmological simulations. Matching both relations requires disk sizes to satisfy constraints given by the concentration of halos and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes ingalaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following pproximatelythe prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. ΛCDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.