2009A&A...504....1H

The aim of the present work is to study the overall mass distribution of the galaxy clusters Abell 1351 and Abell 1995 using weak gravitational lensing. These clusters have a very different mass structure and dynamical state and are the two extremes from a larger sample of 38 X-ray luminous clusters of similar size and redshift. We measure the shear values of faint background galaxies and correct for PSF anisotropies using the KSB+ method. Two-dimensional mass maps of the clusters are created using a finite-field mass reconstruction algorithm, and verified with aperture mass statistics. The masses inferred from the reconstructions are compared to those obtained from fitting spherically symmetric SIS- and NFW-models to the tangential shear profiles. We discuss the NFW concentration parameters in detail. From the mass reconstructions we infer M_2D(<r₂₀₀)-masses of 11.7±3.1x10¹⁴h₇₀^–1M_☉ and 10.5±2.7x10¹⁴h₇₀^–1M_☉ for Abell 1351 and Abell 1995, respectively. About 3' northeast of the main mass peak of Abell 1351, we detect a significant secondary peak both in the mass reconstruction and from aperture mass statistics. This feature is also traced by cluster members selected by means of their V-I colour, and is therefore likely a real substructure of Abell 1351. From our fits to the tangential shear we infer masses of the order of M₂₀₀∼8-9x10¹⁴ h₇₀^–1M_☉ (Abell 1351) and M₂₀₀∼5-6x10¹⁴ h₇₀^–1M_☉ (Abell 1995). The concentration parameters remain poorly constrained by our weak lensing analysis.