Shaping the X-ray spectrum of galaxy clusters with AGN feedback and   turbulence
  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: $dL_{\rm x}/dT \propto (T/T_{\rm hot})^{\alpha=2\pm1}$. 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 $\alpha \simeq 2$, oscillating within the observed $1<\alpha<3$. In the absence of thermal instability, the X-ray spectrum remains isothermal ($\alpha > 8$), while unopposed cooling drives a too shallow slope, $\alpha<1$. AGN outflows deposit their energy inside-out, releasing more heat in the inner cooler phase; radially distributed heating alone induces a declining spectrum, $1<\alpha<2$. 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 $\alpha\approx3$. Self-regulated AGN outflow feedback can address the soft X-ray problem through the interplay of heating and turbulence. 
M. Gaspari
astro-ph.HE astro-ph.CO astro-ph.GA physics.flu-dyn