Selecting background galaxies in weak-lensing analysis of galaxy
  clusters
  In this paper, we present a new method to select the faint, background
galaxies used to derive the mass of galaxy clusters by weak lensing.
  The method is based on the simultaneous analysis of the shear signal, that
should be consistent with zero for the foreground, unlensed galaxies, and of
the colors of the galaxies: photometric data from the COSMic evOlution Survey
are used to train the color selection. In order to validate this methodology,
we test it against a set of state-of-the-art image simulations of mock galaxy
clusters in different redshift [$0.23-0.45$] and mass
[$0.5-1.55\times10^{15}M_\odot$] ranges, mimicking medium-deep multicolor
imaging observations (e.g. SUBARU, LBT).
  The performance of our method in terms of contamination by unlensed sources
is comparable to a selection based on photometric redshifts, which however
requires a good spectral coverage and is thus much more observationally
demanding. The application of our method to simulations gives an average ratio
between estimated and true masses of $\sim 0.98 \pm 0.09$. As a further test,
we finally apply our method to real data, and compare our results with other
weak lensing mass estimates in the literature: for this purpose we choose the
cluster Abell 2219 ($z=0.228$), for which multi-band (BVRi) data are publicly
available.
