Simulations of Quintessential Cold Dark Matter: beyond the cosmological constant

TL;DR

This study uses large N-body simulations to analyze how different quintessence dark energy models influence cosmic structure growth, revealing potential observational signatures that distinguish them from the standard cosmological constant model.

Contribution

It provides the first detailed nonlinear growth analysis of various quintessence models, highlighting their effects on structure formation and potential observational discriminants.

Findings

Quintessence models with late rapid transitions can mimic mbda CDM in BAO peak positions.

Models with late transitions show higher dark matter halo abundance at z>0.

Early transition models are indistinguishable from mbda CDM in mass function and BAO measurements.

Abstract

We study the nonlinear growth of cosmic structure in different dark energy models, using large volume N-body simulations. We consider a range of quintessence models which feature both rapidly and slowly varying dark energy equations of state, and compare the growth of structure to that in a universe with a cosmological constant. The adoption of a quintessence model changes the expansion history of the universe, the form of the linear theory power spectrum and can alter key observables, such as the horizon scale and the distance to last scattering. We incorporate these effects into our simulations in stages to isolate the impact of each on the growth of structure. The difference in structure formation can be explained to first order by the difference in growth factor at a given epoch; this scaling also accounts for the nonlinear growth at the 15% level. We find that quintessence models that are different from $\Lambda$CDM both today and at high redshifts $(z \sim 1000)$ and which feature late $(z<2)$, rapid transitions in the equation of state, can have identical baryonic acoustic oscillation (BAO) peak positions to those in $\Lambda$CDM. We find that these models have higher abundances of dark matter haloes at $z>0$ compared to $\Lambda$CDM and so measurements of the mass function should allow us to distinguish these quintessence models from a cosmological constant. However, we find that a second class of quintessence models, whose equation of state makes an early $(z>2)$ rapid transition to $w=-1$, cannot be distinguished from $\Lambda$CDM using measurements of the mass function or the BAO, even if these models have non-negligible amounts of dark energy at early times.