Weak lensing density profiles and mass reconstructions of the galaxy
  clusters Abell 1351 and Abell 1995
  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 got 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 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 M200-masses of 11.7 +/- 3.1 * 10^14
h_70^-1 Msun and 10.5 +/- 2.7 * 10^14 h_70^-1 Msun for Abell 1351 and Abell
1995, respectively. About 3' north-east of the main mass peak of Abell 1351 we
detect a significant secondary peak in the mass reconstruction as well as by
aperture mass statistics. This feature is also traced by clusters members
selected by means of their V-I colour, and hence is likely a real sub-structure
of Abell 1351. From our fits to the tangential shear we infer masses on the
order of M200 ~ 8-9 * 10^14 h_70^-1 Msun (Abell 1351) and M200 ~ 5-6 * 10^14
h_70^-1 Msun (Abell 1995). The concentration parameters remain poorly
constrained by our weak lensing analysis.
