A large difference in the progenitor masses of active and passive galaxies in the EAGLE simulation

Abstract

Cumulative number density matching of galaxies is a method to observationally connect descendent galaxies to their typical main progenitors at higher redshifts and thereby to assess the evolution of galaxy properties. The accuracy of this method is limited due to galaxy merging and scatter in the stellar mass growth history of individual galaxies. Behroozi et al. (2013) have introduced a refinement of the method, based on abundance matching of observed galaxies to the Bolshoi dark-matter-only simulation. The EAGLE cosmological hydro-simulation is well suited to test this method, because it reproduces the observed evolution of the galaxy stellar mass function and the passive fraction. We find agreement with the Behroozi et al. (2013) method for the complete sample of main progenitors of z = 0 galaxies, but we also find a strong dependence on the current star formation rate. Passive galaxies with a stellar mass up to 10^10.75 Msun have a completely different median mass history than active galaxies of the same mass. This difference persists if we only select central galaxies. This means that the cumulative number density method should be applied separately to active and passive galaxies. Even then, the typical main progenitor of a z = 0 galaxy already spans two orders of magnitude in stellar mass at z = 2.

Accepted for publication in MNRAS Letters, 5 pages, 5 figures

References in corpus (7)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The hierarchical formation of the brightest cluster galaxies
• The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
• It's not easy being green: The evolution of galaxy colour in the EAGLE simulation
• From Diversity to Dichotomy, and Quenching: Milky-Way-Like and Massive-Galaxy Progenitors at 0.5<z<3.0
• Tracing galaxy populations through cosmic time: A critical test of methods for connecting the same galaxies between different redshifts at $z<3$
• The Diversity of Growth Histories of Milky Way-mass Galaxies

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