Observational constraints on the redshift evolution of X-ray scaling
  relations of galaxy clusters out to z ~ 1.5
  A precise understanding of the relations between observable X-ray properties
of galaxy clusters and cluster mass is a vital part of the application of X-ray
galaxy cluster surveys to test cosmological models. An understanding of how
these relations evolve with redshift is just emerging from a number of
observational data sets.
  The current literature provides a diverse and inhomogeneous picture of
scaling relation evolution. We attempt to transform these results and the data
on recently discovered distant clusters into an updated and consistent
framework, and provide an overall view of scaling relation evolution.
  We study in particular the M-T, L_X-T, and M-L_X relation combining 14
published data sets supplemented with recently published data of distant
clusters and new results from follow-up observations of the XMM-Newton Distant
Cluster Project (XDCP).
  We find that the evolution of the M-T relation is consistent with the
self-similar prediction, while the evolution of X-ray luminosity for a given
temperature and mass for a given X-ray luminosity is slower than predicted. Our
best fit results for the evolution factor E(z)^alpha are alpha = -1.04+-0.07
for the M-T relation, alpha = -0.23+0.12-0.62 for the L-T relation, and alpha =
-0.93+0.62-0.12 for the M-L_X relation. We find that selection biases are the
most likely reason for apparent inconsistencies between different published
data sets.
  The new results provide the currently most robust calibration of
high-redshift cluster mass estimates based on X-ray luminosity and temperature
and help us to improve the prediction of the number of clusters to be found in
future galaxy cluster X-ray surveys, such as eROSITA. The comparison of
evolution results with hydrodynamical cosmological simulations suggests that
early preheating of the intracluster medium provides the most suitable scenario
to explain the observed evolution.
