Cluster halo shapes in CDM and SIDM models: Unveiling the DM particle nature using a weak lensing approach

TL;DR

This study uses galaxy-galaxy lensing of simulated data to distinguish between CDM and SIDM models by analyzing the shapes and elongations of galaxy cluster halos, revealing differences in their radial shape profiles.

Contribution

It introduces a novel lensing-based method to measure halo shapes and differentiate dark matter models through detailed shape analysis of simulated halos.

Findings

SIDM halos are rounder towards the center compared to CDM halos.

Shape profiles show a higher slope for SIDM halos, indicating radial shape variation.

Large-scale structure influences halo elongation differently in SIDM and CDM models.

Abstract

Self-interacting dark matter (SIDM) is an alternative to the standard collisionless cold dark matter model (CDM), allowing for interactions between the dark matter particles through the introduction of a self-scattering cross-section. However, the observable effects between these two scenarios are hard to detect. In this work we present a detailed analysis of an application of galaxy-galaxy lensing to measure with high precision the shapes of cluster halos and how this approach can be used to obtain information regarding the nature of the dark matter particle. Using two sets of simulated data, SIDM and CDM simulations, we compute stacked shear maps centred on several subsets of halos with masses $\gtrsim 10^{13.5} M_\odot$. From these maps, we obtain the quadrupole profiles related to the mean projected elongation of the particle distribution from which the shape parameters are derived. Accounting for a radial shape variation, this technique provides an enhancement of the observed differences between the simulated data-sets. In particular, we obtain a higher slope of the power law for the shape-radial relation for the halos identified in the SIDM simulation, which are rounder towards the centre. Also, as approaching to the mean virial radius, the projected semi-axis ratios converge to similar values than in the CDM simulation. Moreover, we account for the impact of the neighbouring mass, where more strongly elongated distributions are found for the halos in the SIDM simulation, indicating that under dark matter self interaction, the large scale structure imprints a more coherent accretion process.