The effects of baryonic cooling on the concentration-mass relation

TL;DR

This paper investigates how baryonic cooling influences the concentration-mass relation in galaxy groups and clusters, showing that including baryons and their contraction effects aligns models more closely with observations.

Contribution

It introduces a simple spherical halo model incorporating stars, gas, and baryonic contraction to better match observed concentration-mass relations.

Findings

Baryonic effects steepen the concentration-mass relation.

Including baryons improves the match with observational data.

Baryon redistribution can also produce similar effects.

Abstract

I re-examine the relation between virial mass and concentration for groups and clusters of galaxies as measured in a number of recent works. As previously noted by several authors, low-mass clusters and groups of galaxies display systematically larger concentrations than simple prescriptions based on pure $n$-body simulations would predict. This implies an observed concentration-mass relation with a substantially larger slope/normalization than expected from theoretical investigations. Additionally, this conclusion seems to be quite independent on selection effects, holding for both lensing based and X-ray based cluster samples. In order to shed new light on this issue I employ a simple spherical halo model containing, in addition to dark matter, also stars and hot diffuse gas in proportions and with distributions in agreement with the most recent observations. Moreover, I include the contraction effect experienced by dark matter due to the cooling of baryons in the very central part of the structure itself. The resulting modified concentration-mass relation is steeper than the theoretical input one, because star formation is fractionally more efficient in low-mass objects. However, the effect is non-vanishing at all masses, thus resulting also in a larger normalization. Overall the new relation provides a better representation of the observed one for almost all catalogs considered in this work, although the specific details depend quite significantly on the baryon fraction prescription adopted. Anyhow, the same effect could also be produced by a redistribution of baryons within the structure. Finally I use this simple model to show how the estimated concentration of cosmic structures is expected to be overestimated as a function of the radial range covered by the analysis. (abridged)