Truong, N.; Rasia, E.; Mazzotta, P.; Planelles, S.; Biffi, V.; Fabjan, D.; Beck, Alexander M.; Borgani, Stefano; Dolag, Klaus; Gaspari, M.; Granato, G. L.; Murante, G.; RagoneFigueroa, Cinthia ORCID: 0000000328264799; Steinborn, Lisa K.
(2018):
Cosmological hydrodynamical simulations of galaxy clusters. Xray scaling relations and their evolution.
In: Monthly Notices of the Royal Astronomical Society, Vol. 474, No. 3: pp. 40894111

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Abstract
We analyse cosmological hydrodynamical simulations of galaxy clusters to study the Xray scaling relations between total masses and observable quantities such as Xray luminosity, gas mass, Xray temperature, and YX. Three sets of simulations are performed with an improved version of the smoothed particle hydrodynamics GADGET3 code. These consider the following: nonradiative gas, star formation and stellar feedback, and the addition of feedback by active galactic nuclei (AGN). We select clusters with M500 > 10(14) M circle dot E(z)(1), mimicking the typical selection of SunyaevZeldovich samples. This permits to have a mass range large enough to enable robust fitting of the relations even at z similar to 2. The results of the analysis show a general agreement with observations. The values of the slope of the massgas mass and masstemperature relations at z = 2 are 10 per cent lower with respect to z = 0 due to the applied mass selection, in the former case, and to the effect of early merger in the latter. We investigate the impact of the slope variation on the study of the evolution of the normalization. We conclude that cosmological studies through scaling relations should be limited to the redshift range z = 01, where we find that the slope, the scatter, and the covariance matrix of the relations are stable. The scaling between mass and YX is confirmed to be the most robust relation, being almost independent of the gas physics. At higher redshifts, the scaling relations are sensitive to the inclusion of AGNs which influences lowmass systems. The detailed study of these objects will be crucial to evaluate the AGN effect on the ICM.