We present a consistent analysis of Chandra and XMM-Newton observations of an approximately mass-selected sample of 50 galaxy clusters at 0.15 < z < 0.3 – the “ LoCuSS High- L _ { X } Sample ” .
We apply the same analysis methods to data from both satellites , including newly developed analytic background models that predict the spatial variation of the Chandra and XMM-Newton backgrounds to < 2 \% and < 5 \% precision respectively .
To verify the cross-calibration of Chandra - and XMM-Newton -based cluster mass measurements , we derive the mass profiles of the 21 clusters that have been observed with both satellites , extracting surface brightness and temperature profiles from identical regions of the respective datasets .
We obtain consistent results for the gas and total hydrostatic cluster masses : the average ratio of Chandra - to XMM-Newton -based measurements of M _ { gas } and M _ { X } at r _ { 500 } are 0.99 \pm 0.02 and 1.02 \pm 0.05 , respectively with an intrinsic scatter of \sim 3 \% for gas masses and \sim 8 \% for hydrostatic masses .
Comparison of our hydrostatic mass measurements at r _ { 500 } with the latest LoCuSS weak-lensing results indicate that the data are consistent with non-thermal pressure support at this radius of \sim 7 \% .
We also investigate the scaling relation between our hydrostatic cluster masses and published integrated Compton parameter \mathrel { Y _ { sph } } measurements from the Sunyaev-Zel ’ dovich Array .
We measure a scatter in mass at fixed \mathrel { Y _ { sph } } of \sim 16 \% at \Delta = 500 , which is consistent with theoretical predictions of \sim 10 - 15 \% scatter .