Dissecting the Strong-lensing Galaxy Cluster MS 0440.5+0204. I. The Mass Density Profile

TL;DR

This study models the mass density profile of galaxy cluster MS 0440.5+0204 using strong lensing, dynamical, and weak lensing data, achieving precise mass estimates and comparing well with X-ray measurements.

Contribution

It introduces a combined modeling approach integrating strong lensing, dynamical, and weak lensing data for detailed mass profile analysis of a galaxy cluster.

Findings

Accurate mass profile parameters with reduced uncertainties.

Good agreement between lensing-derived and X-ray mass estimates.

Enhanced constraints on the cluster's scale radius and velocity dispersion.

Abstract

We present a parametric strong lensing modeling of the galaxy cluster MS\,0440.5+0204 (located at $z$ = 0.19). We have performed a strong lensing mass reconstruction of the cluster using three different models. The first model uses the image positions of four multiple imaged systems (providing 26 constraints). The second one combines strong lensing constraints with dynamical information (velocity dispersion) of the cluster. The third one uses the mass calculated from weak lensing as an additional constraint. Our three models reproduce equally well the image positions of the arcs, with a root-mean-square image equal to $\approx$0.5$\arcsec$. However, in the third model, the inclusion of the velocity dispersion and the weak-lensing mass allows us to obtain better constraints in the scale radius and the line-of-sight velocity dispersion of the mass profile. For this model, we obtain $r_s$ = 132$^{+30}_{-32}$ kpc, $\sigma_s$ = 1203$^{+46}_{-47}$ km s$^{-1}$, M$_{200}$ = 3.1$^{+0.6}_{-0.6}$ $\times10^{14}$\,M$_{\odot}$, and a high concentration, $c_{200}$ = 9.9$^{+2.2}_{-1.4}$. Finally, we used our derived mass profile to calculate the mass up to 1.5 Mpc. We compare it with X-ray estimates previously reported, finding a good agreement.