Shaping the X-ray spectrum of galaxy clusters with AGN feedback and turbulence

Abstract

The hot plasma filling galaxy clusters emits copious X-ray radiation. The classic unheated and unperturbed cooling flow model predicts dramatic cooling rates and an isobaric X-ray spectrum with constant differential luminosity distribution. The observed cores of clusters (and groups) show instead a strong deficit of soft X-ray emission: $dL_{\rm x}/dT \propto (T/T_{\rm hot})^{α=2\pm1}$. Using 3D hydrodynamic simulations, we show that such deficit arises from the tight self-regulation between thermal instability condensation and AGN outflow injection: condensing clouds boost the AGN outflows, which quench cooling as they thermalize through the core. The resultant average distribution slope is $α\simeq 2$, oscillating within the observed $1<α<3$. In the absence of thermal instability, the X-ray spectrum remains isothermal ($α> 8$), while unopposed cooling drives a too shallow slope, $α<1$. AGN outflows deposit their energy inside-out, releasing more heat in the inner cooler phase; radially distributed heating alone induces a declining spectrum, $1<α<2$. Turbulence further steepens the spectrum and increases the scatter: the turbulent Mach number in the hot phase is subsonic, while it becomes transonic in the cooler phase, making perturbations to depart from the isobaric mode. Such increase in $d\ln P/d\ln T$ leads to $α\approx3$. Self-regulated AGN outflow feedback can address the soft X-ray problem through the interplay of heating and turbulence.

5 pages, 2 figures, published in MNRAS Letters