Raytracing simulations of coupled dark energy models

TL;DR

This paper investigates how coupled dark energy models affect weak lensing signals by simulating and comparing them to the standard $\\Lambda$CDM model, revealing significant differences in power spectra due to growth of perturbations and non-linear effects.

Contribution

It provides the first detailed raytracing simulations of weak lensing in coupled dark energy models, highlighting their distinct signatures compared to standard cosmology.

Findings

Differences in power spectra up to 40% for extreme models.

Enhanced growth of perturbations in coupled models.

Friction term effects reduce overall lensing signal.

Abstract

Dark matter and dark energy are usually assumed to couple only gravitationally. An extension to this picture is to model dark energy as a scalar field coupled directly to cold dark matter. This coupling leads to new physical effects, such as a fifth-force and a time-dependent dark matter particle mass. In this work we examine the impact that coupling has on weak lensing statistics by constructing realistic simulated weak-lensing maps using raytracing techniques through N-body cosmological simulations. We construct maps for different lensing quantities, covering a range of scales from a few arcminutes to several degrees. The concordance $\Lambda$CDM model is compared to different coupled dark energy models, described either by an exponential scalar field potential (standard coupled dark energy scenario) or by a SUGRA potential (bouncing model). We analyse several statistical quantities and our results, with sources at low redshifts are largely consistent with previous work on CMB lensing by Carbone et al., 2013. The most significant differences from the $\Lambda$CDM model are due to the enhanced growth of the perturbations and to the effective friction term in non-linear dynamics. For the most extreme models, we see differences in the power spectra up to 40% compared to the $\Lambda$CDM model. The different time evolution of the linear matter overdensity can account for most of the differences, but when controlling for this using a $\Lambda$CDM model having the same normalization, the overall signal is smaller due to the effect of the friction term appearing in the equation of motion for dark matter particles.