  We present a method to recover mass profiles of galaxy clusters by combining
data on thermal Sunyaev-Zeldovich (tSZ) and X-ray imaging, thereby avoiding to
use any information on X-ray spectroscopy. This method, which represents a
development of the geometrical deprojection technique presented in Ameglio et
al. (2007), implements the solution of the hydrostatic equilibrium equation. In
order to quantify the efficiency of our mass reconstructions, we apply our
technique to a set of hydrodynamical simulations of galaxy clusters. We propose
two versions of our method of mass reconstruction. Method 1 is completely
model-independent, while Method 2 assumes instead the analytic mass profile
proposed by Navarro et al. (1997) (NFW). We find that the main source of bias
in recovering the mass profiles is due to deviations from hydrostatic
equilibrium, which cause an underestimate of the mass of about 10 per cent at
r_500 and up to 20 per cent at the virial radius. Method 1 provides a
reconstructed mass which is biased low by about 10 per cent, with a 20 per cent
scatter, with respect to the true mass profiles. Method 2 proves to be more
stable, reducing the scatter to 10 per cent, but with a larger bias of 20 per
cent, mainly induced by the deviations from equilibrium in the outskirts. To
better understand the results of Method 2, we check how well it allows to
recover the relation between mass and concentration parameter. When analyzing
the 3D mass profiles we find that including in the fit the inner 5 per cent of
the virial radius biases high the halo concentration. Also, at a fixed mass,
hotter clusters tend to have larger concentration. Our procedure recovers the
concentration parameter essentially unbiased but with a scatter of about 50 per
cent.
