The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

Abstract

We study the redshift evolution of the X-ray and Sunyaev-Zel'dovich (SZ) scaling relations for galaxy groups and clusters in the fable suite of cosmological hydrodynamical simulations. Using an expanded sample of 27 high-resolution zoom-in simulations, together with a uniformly-sampled cosmological volume to sample low-mass systems, we find very good agreement with the majority of observational constraints up to z ∼ 1. We predict significant deviations of all examined scaling relations from the simple self-similar expectations. While the slopes are approximately independent of redshift, the normalisations evolve positively with respect to self-similarity, even for commonly-used mass proxies such as the Y X parameter. These deviations are due to a combination of factors, including more effective AGN feedback in lower mass haloes, larger binding energy of gas at a given halo mass at higher redshifts and larger nonthermal pressure support from kinetic motions at higher redshifts. Our results have important implications for cluster cosmology from upcoming SZ surveys such as SPT-3G, ACTpol and CMB-S4, as relatively small changes in the observable-mass scaling relations (within theoretical uncertainties) have a large impact on the predicted number of high-redshift clusters and hence on our ability to constrain cosmology using cluster abundances. In addition, we find that the intrinsic scatter of the relations, which agrees well with most observational constraints, increases at lower redshifts and for lower mass systems. This calls for a more complex parametrization than adopted in current observational studies to be able to accurately account for selection biases.

Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

“…At higher radii the curves of radio and nonradio BGGs decrease in a similar fashion, while the probability density of simulated BGGs already steepens at ∼ 0.1 Rvir. Nevertheless, in simulations BGGs tend to be more massive than their observational counterparts (e.g., Bahé et al, 2017;Henden et al, 2019;Bassini et al, 2020). For this reason, they are closer to the centre and exhibit less spread in velocity.…”

On the Origin and Evolution of the Intra-Cluster Light: A Brief Review of the Most Recent Developments

“…There is no general agreement of a possible dependence of f ICL on cluster mass among different studies, both observational and theoretical ( [4,10,14,16,17,24,31,33,49,53,54,60,78,96,97,109,110,[128][129][130][131] just to quote some theoretical and the most recent observational studies). Some theoretical works (e.g., [49,55,130,132]) find an increasing f ICL with cluster mass, others (e.g., [4,18,20]) no relation, and others (e.g., [14]) a slight decreasing f ICL with increasing cluster mass.…”

“…There is no general agreement of a possible dependence of f ICL on cluster mass among different studies, both observational and theoretical ( [4,10,14,16,17,24,31,33,49,53,54,60,78,96,97,109,110,[128][129][130][131] just to quote some theoretical and the most recent observational studies). Some theoretical works (e.g., [49,55,130,132]) find an increasing f ICL with cluster mass, others (e.g., [4,18,20]) no relation, and others (e.g., [14]) a slight decreasing f ICL with increasing cluster mass. Overall, by collecting all the results so far obtained and considering the scatter, f ICL is found to be independent on halo mass, and range between ∼5% (group scale, lower limit) and ∼50% (cluster scale, upper limit) at the present day (I refer those readers interested in a collection of the most recent f ICL derived in observed and simulated objects to Tang et al [17], Furnell et al [24], Kluge et al [33], Ragusa et al [96]), with a quite large scatter over the whole halo mass range probed.…”

The Fornax Deep Survey with VST

“…Clusters of galaxies are expected to grow over time by accreting smaller groups. During the infall process, the material stripped from the galaxy outskirts builds up the intra-cluster light (ICL; see Napolitano et al 2003;Contini et al 2014Contini et al , 2019Cui et al 2014;Pillepich et al 2018;DeMaio et al 2018;Henden et al 2019). The ICL is the fossil record of all past interactions and mergers.…”