Proca-stinated Cosmology I: A N-body code for the vector Galileon

TL;DR

This paper develops and tests a modified N-body simulation code for the cubic vector Galileon model, exploring how the model's parameters influence structure formation and screening effects in cosmology.

Contribution

It introduces a new N-body code incorporating the vector Galileon theory with screening effects, and analyzes the impact of model parameters on cosmic structure growth.

Findings

Transverse mode has negligible impact on structure formation.

The parameter beta_3 controls the strength of the fifth force and screening effectiveness.

The model interpolates between scalar Galileon and quintessence behaviors.

Abstract

We investigate the nonlinear growth of large-scale structure in the generalised Proca theory, in which a self-interacting massive vector field plays the role of driving the acceleration of the cosmic expansion. Focusing to the Proca Lagrangian at cubic order -- the cubic vector Galileon model -- we derive the simplified equations for gravity as well as the longitudinal and transverse modes of the vector field under the weak-field and quasi-static approximations, and implement them in a modified version of the ECOSMOG N-body code. Our simulations incorporate the Vainshtein screening effect, which reconciles the fifth force propagated by the longitudinal mode of the cubic vector Galileon model with local tests of gravity. The results confirm that for all scales probed by the simulation, the transverse mode has a negligible impact on structure formation in a realistic cosmological setup. It is well known that in this model the strength of the fifth force is controlled by a free model parameter, which we denote as beta_3. By running a suite of cosmological simulations for different values of beta_3, we show that this parameter also determines the effectiveness of the Vainshtein screening. The model behaves identically to the cubic scalar Galileon for beta_3 going to zero, in which the fifth force is strong in unscreened regions but is efficiently screened in high-density regions. In the opposite limit, beta_3 going to infinity, the model approaches its `quintessence' counterpart, which has a vanishing fifth force but a modified expansion history compared to LambdaCDM. This endows the model with rich phenomenology, which will be investigated in future works.