The evolution of galaxy cluster X-ray scaling relations

TL;DR

This paper uses advanced simulations to study how feedback from supernovae and active galactic nuclei influences the evolution of galaxy cluster X-ray scaling relations, comparing models with observations.

Contribution

It introduces a hybrid feedback model based on galaxy formation semi-analytic models and compares its predictions with a simple preheating model, highlighting differences in evolutionary behavior.

Findings

Feedback model reproduces local X-ray scaling laws for non-cool core clusters.

Models predict opposing evolution at high redshift.

Observations favor feedback model at z<0.5, preheating at higher redshift.

Abstract

We use numerical simulations to investigate, for the first time, the joint effect of feedback from supernovae (SNe) and active galactic nuclei (AGN) on the evolution of galaxy cluster X-ray scaling relations. Our simulations are drawn from the Millennium Gas Project and are some of the largest hydrodynamical N-body simulations ever carried out. Feedback is implemented using a hybrid scheme, where the energy input into intracluster gas by SNe and AGN is taken from a semi-analytic model of galaxy formation. This ensures that the source of feedback is a population of galaxies that closely resembles that found in the real universe. We show that our feedback model is capable of reproducing observed local X-ray scaling laws, at least for non-cool core clusters, but that almost identical results can be obtained with a simplistic preheating model. However, we demonstrate that the two models predict opposing evolutionary behaviour. We have examined whether the evolution predicted by our feedback model is compatible with observations of high-redshift clusters. Broadly speaking, we find that the data seems to favour the feedback model for z<0.5, and the preheating model at higher redshift. However, a statistically meaningful comparison with observations is impossible, because the large samples of high-redshift clusters currently available are prone to strong selection biases. As the observational picture becomes clearer in the near future, it should be possible to place tight constraints on the evolution of the scaling laws, providing us with an invaluable probe of the physical processes operating in galaxy clusters.