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In Schneider, King & Erben (2000) we developed likelihood techniques tocompare the constraints on cluster mass profiles that can be obtained using theshear and magnification information. This work considered circularly symmetricpower-law models for clusters at fairly low redshifts where the redshiftdistribution of source galaxies could be neglected. Here this treatment isextended to encompass NFW profiles which are a good description of clustersfrom cosmological N-body simulations, and NFW clusters at higher redshiftswhere the influence of various scenarios for the knowledge of the redshiftdistribution are examined. Since in reality the overwhelming majority ofclusters have ellipsoidal rather than spherical profiles, the singularisothermal ellipsoid (SIE) is investigated. We also briefly consider the impactof substructure on such a likelihood analysis. In general, we find that theshear information provides a better constraint on the NFW profile underconsideration, so this becomes the focus of what follows. The ability todifferentiate between the NFW and power-law profiles strongly depends on thesize of the data field, and on the number density of galaxies for which anellipticity can be measured. For higher redshift NFW profiles, there is verylittle reduction (~1.5%) in the dispersion of parameter estimates whenspectroscopic redshifts, as opposed to photometric redshift estimates, areavailable for the galaxies used in the lensing analysis.Comment: 15 pages, Submitted to A&

Cluster mass profiles from weak lensing II