# Halo Concentrations and the New Baseline X-ray Luminosity-Temperature and Mass Relations of Galaxy Clusters

## TL;DR

This paper revises the baseline X-ray luminosity-temperature and mass relations of galaxy clusters by incorporating the effects of halo concentration, predicting shallower slopes than traditional models, and confirms these predictions with simulations.

## Contribution

It introduces new baseline relations for galaxy cluster X-ray luminosity and mass that account for halo concentration effects, challenging previous predictions.

## Key findings

- Predicted $L_X$-$T_X$ relation slope is ~1.7, shallower than 2.
- Numerical simulations find $L_X$-$T_X$ slope around 1.6.
- Baseline $L_X$-$M_\Delta$ relation slope is ~1.1-1.2, less than 4/3.

## Abstract

The standard self-similar model of galaxy cluster formation predicts that the X-ray luminosity-temperature ($L_X$-$T_X$) relation of galaxy clusters should have been $L_X\propto T_X^2$ in absence of the baryonic physics, such as radiative cooling and feedback from stars and black holes. However, this baseline relation is predicted without considering the fact that the halo concentration and the characteristic density of clusters increases as their mass decreases, which is a consequence of hierarchical structure formation of the universe. Here, we show that the actual baseline relation should be $L_X\propto T_X^\alpha$, where $\alpha\sim 1.7$, instead of $\alpha=2$, given the mass dependence of the concentration and the fundamental plane relation of galaxy clusters. Numerical simulations show that $\alpha\sim 1.6$, which is consistent with the prediction. We also show that the baseline luminosity-mass ($L_X$-$M_\Delta$) relation should have been $L_X\propto M_\Delta^\beta$, where $\beta\sim 1.1$-1.2, in contrast with the conventional prediction ($\beta=4/3$). In addition, some of the scatter in the $L_X$-$M_\Delta$ relation can be attributed to the scatter in the concentration-mass ($c$-$M$) relation. The confirmation of the shallow slope could be a proof of hierarchical clustering. As an example, we show that the new baseline relations could be checked by studying the temperature or mass dependence of gas mass fraction of clusters. Moreover, the highest-temperature clusters would follow the shallow baseline relations if the influences of cool cores and cluster mergers are properly removed.