to the amplitude of the X-ray hydrostatic mass bias derived both in observations [@vonderlinden.etal.2014; @maughan.etal.2015] and simulations [@2007ApJ...655...98N; @2012NJPh...14e5018R; @biffi.etal.2016], we prefer to refer to masses estimated via the gravitational lensing technique. More specifically, we refer to [@2013ApJ...767..116M], [@kettula.etal.2013], and [@2015arXiv151203857L]. The first sample contains 50 galaxy clusters in the redshift range $0.155<z<0.55$. The optical data are taken from the Canadian Clusters Comparison Project (CCCP, see @hoekstra.etal.2015), while the X-ray properties are based on the combined data from the $Chandra$ Observatory and the $XMM-Newton$ telescope. [@kettula.etal.2013] analyze 10 groups with redshifts between 0.1 and 0.8 taken from the COSMOS field and observed by the Hubble Space Telescope and the XMM-Newton telescope. [@2015arXiv151203857L] provides X-ray observations of 38 clusters with $z<0.6$ as part of the XXL survey. These data are associated with independent mass measurements from the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS, e.g. @2012MNRAS.427..146H; @2013MNRAS.433.2545E). The temperature measurements are restricted to the inner 300 kpc of each object.

Comparison to Observations at local and intermediate redshifts
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[![image](fig2a){width="40.00000%"}]{} [![image](fig2b){width="40.00000%"}]{} [![image](fig2c){width="40.00000%"}]{} [![image](fig2d){width="40.00000%"}]{}

![image](fig3a){width="40.00000%"} ![image](fig3b){width="40.00000%"} ![image](fig3c){width="40.00000%"} ![image](fig3d){width="40.00000%"}

![The $z=0$ [[[agn]{}]{}]{} simulated luminosity-temperature relation is shown in blue and black asterisks, respectively, for cool-core and non-cool-core systems [@2015ApJ...813L..17R]. For comparison, the cool-core and non-cool-core 