Dark Matter in ms1224 from Distortion of Background Galaxies
  We explore the dark matter distribution in ms1224.7+2007 using the gravitational distortion of the images of faint background galaxies. Projected mass image reconstruction reveals a highly significant concentration coincident with the X-ray and optical location. The concentration is seen repeatably in reconstructions from independent subsamples and the azimuthally averaged tangential shear pattern is also clearly seen in the data. The projected mass within a $2.76'$ radius aperture is $\simeq 3.5 \times 10^{14} h^{-1} M_{\sun}$. This is $\simeq 3$ times larger than that predicted if mass traces light with $M/L = 275 h$ as derived from virial analysis. It is very hard to attribute the discrepancy to a statistical fluctuation, and a further indication of a significant difference between the mass and the light comes from a second mass concentration which is again seen in independent subsamples but which is not seen at all in the cluster light. We find a mass per galaxy visible to $I = 22$ of $\simeq 8 \times 10^{12}h^{-1}M_{\sun}$ which, if representative of the universe, implies a density parameter $\Omega \sim 2$. We find a null detection of any net shear from large-scale structure with a precision of 0.9\% per component. This is much smaller than the possible detection in a recent comparable study, and the precision here is comparable to to the minimum level of rms shear fluctuations implied by observed large-scale structure. 
G.G. Fahlman, Nick Kaiser, Gordon Squires and David Woods