AMICO galaxy clusters in KiDS-DR3: weak-lensing mass calibration

TL;DR

This paper calibrates galaxy cluster masses using weak lensing in KiDS-DR3, establishing relations between mass and two cluster proxies, A and λ*, across a broad mass range and redshift span.

Contribution

It provides the first weak lensing mass calibration for AMICO-detected clusters in KiDS-DR3, linking observables to halo mass over a wide mass and redshift range.

Findings

Established A-M200 relation with a slope of ~2.0.

Derived λ*-M200 relation with a slope of ~1.7.

Confirmed small redshift evolution in the relations.

Abstract

We present the mass calibration for galaxy clusters detected with the AMICO code in KiDS DR3 data. The cluster sample comprises $\sim$ 7000 objects and covers the redshift range 0.1 < $z$ < 0.6. We perform a weak lensing stacked analysis by binning the clusters according to redshift and two different mass proxies provided by AMICO, namely the amplitude $A$ (measure of galaxy abundance through an optimal filter) and the richness $\lambda^*$ (sum of membership probabilities in a consistent radial and magnitude range across redshift). For each bin, we model the data as a truncated NFW profile plus a 2-halo term, taking into account uncertainties related to concentration and miscentring. From the retrieved estimates of the mean halo masses, we construct the $A$-$M_{200}$ and the $\lambda^*$-$M_{200}$ relations. The relations extend over more than one order of magnitude in mass, down to $M_{200} \sim 2 (5) \times 10^{13} M_\odot/h$ at $z$ = 0.2 (0.5), with small evolution in redshift. The logarithmic slope is $\sim 2.0$ for the $A$-mass relation, and $\sim 1.7$ for the $\lambda^*$-mass relation, consistent with previous estimations on mock catalogues and coherent with the different nature of the two observables.