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

TL;DR

This study uses the EAGLE cosmological simulations to analyze the Tully-Fisher relation, demonstrating that galaxy sizes, halo properties, and abundance matching models collectively explain the observed mass-velocity scaling and its weak evolution over time.

Contribution

It shows that EAGLE simulations can reproduce the Tully-Fisher relation and its evolution by incorporating galaxy size constraints and abundance matching, providing insights into galaxy-halo connections.

Findings

EAGLE galaxies match observed TFR with tight mass-velocity scaling.

Galaxy sizes and halo properties are crucial for reproducing the TFR.

Weak TFR evolution is consistent with abundance matching models.

Abstract

The Tully-Fisher relation (TFR) links the stellar mass of a disk galaxy, $M_{\rm str}$, 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 mass-velocity scaling ($M\propto V^3$) of dark matter halos, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to be non-monotonic and rapidy evolving. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of $\Lambda$CDM 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 in galaxy 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 approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to $z=1$. $\Lambda$CDM 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.