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We use gas-dynamical simulations of galaxy clusters to compare their X-rayand strong lensing properties. Special emphasis is laid on mass estimates. Thecluster masses range between 6 x 10^14 solar masses and 4 x 10^15 solar masses,and they are examined at redshifts between 1 and 0. We compute the X-rayemission of the intracluster gas by thermal bremsstrahlung, add backgroundcontamination, and mimic imaging and spectral observations with current X-raytelescopes. Although the beta model routinely provides excellent fits to theX-ray emission profiles, the derived masses are typically biased low because ofthe restricted range of radii within which the fit can be done. For beta valuesof ~ 2/3, which is the average in our numerically simulated sample, the mass istypically underestimated by ~ 40 per cent. The masses of clusters which exhibitpronounced substructure are often substantially underestimated. We suggest thatthe ratio between peak temperature and emission-weighted average clustertemperature may provide a good indicator for ongoing merging and, therefore,for unreliable mass estimates. X-ray mass estimates are substantially improvedif we fit a King density profile rather than the beta model to the X-rayemission, thereby dropping the degree of freedom associated with beta. Clustersselected for their strong lensing properties are typically dynamically moreactive than typical clusters. Bulk flows in the intracluster gas contain alarger than average fraction of the internal energy of the gas in such objects,hence the measured gas temperatures are biased low. The bulk of the opticaldepth for arc formation is contributed by clusters with intermediate ratherthan high X-ray luminosity. Arcs occur predominantly in clusters which exhibitsubstructure and are not in an equilibrium state. Finally we explain why theComment: 22 pages including figures, submitted to MNRA

A comparison of X-ray and strong lensing properties of simulated X-ray clusters