Implications of the universal temperature profile for galaxy clusters

We study the X‐ray cluster gas density distribution in hydrostatic equilibrium using the universal temperature profile obtained from recent simulations involving only gravitational processes. If this temperature profile is an indicator of the influence of gravitational processes alone on the intracluster medium (ICM), then the comparison of various X‐ray parameters expected from this profile and the observed data would point towards any additional physics that may be required. We compare the entropy at 0.1 R 200 and R 500 , the scaled entropy profile, the gas fraction at 0.3 R 200 and the gas fraction profile with recent observations and we discuss the implications of this temperature profile in light of these data. We find that the entropy imparted to the gas from gravitational processes alone is larger than previously thought. The entropy at R 500 for rich clusters is consistent with the data, whereas the entropy at 0.1 R 200 is still less than the observed values. We also find that the gas fraction in the inner region of clusters, expected from gravitational processes alone, is smaller than previously thought but larger than the observed data. It does show a trend with the emission‐weighted temperature (〈 T 〉) as shown by the data. We therefore find that the role of any additional non‐gravitational process influencing the physical state of ICM would have to be revised in light of these findings.