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We use the cosmo-OWLS suite of cosmological hydrodynamical simulations toinvestigate the scatter and evolution of the global hot gas properties of largesimulated populations of galaxy groups and clusters. Our aim is to compare thepredictions of different physical models and to explore the extent to whichcommonly-adopted assumptions in observational analyses (e.g. self-similarevolution) are violated. We examine the relations between (true) halo mass andthe X-ray temperature, X-ray luminosity, gas mass, Sunyaev-Zel'dovich (SZ)flux, the X-ray analogue of the SZ flux ($Y_X$) and the hydrostatic mass. Forthe most realistic models, which include AGN feedback, the slopes of thevarious mass-observable relations deviate substantially from the self-similarones, particularly at late times and for low-mass clusters. The amplitude ofthe mass-temperature relation shows negative evolution with respect to theself-similar prediction (i.e. slower than the prediction) for all models,driven by an increase in non-thermal pressure support at higher redshifts. TheAGN models predict strong positive evolution of the gas mass fractions at lowhalo masses. The SZ flux and $Y_X$ show positive evolution with respect toself-similarity at low mass but negative evolution at high mass. The scatterabout the relations is well approximated by log-normal distributions, withwidths that depend mildly on halo mass. The scatter decreases significantlywith increasing redshift. The exception is the hydrostatic mass-halo massrelation, for which the scatter increases with redshift. Finally, we discussthe relative merits of various hot gas-based mass proxies.

The scatter and evolution of the global hot gas properties of simulated galaxy cluster populations