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In this paper we use deep CFHT and SUBARU $uBVRIz$ archival images of theAbell 383 cluster (z=0.187) to estimate its mass by weak lensing. To this end,we first use simulated images to check the accuracy provided by our KSBpipeline. Such simulations include both the STEP 1 and 2 simulations, and morerealistic simulations of the distortion of galaxy shapes by a cluster with aNavarro-Frenk-White (NFW) profile. From such simulations we estimate the effectof noise on shear measurement and derive the correction terms. The R-band imageis used to derive the mass by fitting the observed tangential shear profilewith a NFW mass profile. Photometric redshifts are computed from the uBVRIzcatalogs. Different methods for the foreground/background galaxy selection areimplemented, namely selection by magnitude, color and photometric redshifts,and results are compared. In particular, we developed a semi-automaticalgorithm to select the foreground galaxies in the color-color diagram, basedon observed colors. Using color selection or photometric redshifts improves thecorrection of dilution from foreground galaxies: this leads to higher signalsin the inner parts of the cluster. We obtain a cluster mass that is ~ 20%higher than previous estimates, and is more consistent the mass expected fromX--ray data. The R-band luminosity function of the cluster is finally computed.

A weak lensing analysis of the Abell 383 cluster