We measure the mass distribution of galaxy cluster Abell 1689 within 0.3 Mpc/h _ { 70 } of the cluster centre using its strong lensing effect on 32 background galaxies , which are mapped in altogether 107 multiple images .
The multiple images are based on those of with modifications to both include new and exclude some of the original image systems .
The cluster profile is explored further out to \sim 2.5 Mpc/h _ { 70 } with weak lensing shear measurements from .

The masses of \sim 200 cluster galaxies are measured with Fundamental Plane in order to accurately model the small scale mass structure in the cluster .
The cluster galaxies are modelled as elliptical truncated isothermal spheres .
The scaling of the truncation radii with the velocity dispersions of galaxies are assumed to match those of i ) field galaxies ( ) and ii ) theoretical expectations for galaxies in dense environments ( ) .
The dark matter component of the cluster is described by either non-singular isothermal ellipsoids ( NSIE ) or elliptical versions of the universal dark matter profile ( ENFW ) .
To account for substructure in the dark matter we allow for two dark matter haloes .

The fitting of a single isothermal sphere to the smooth DM component results in a velocity dispersion of 1450 ^ { +39 } _ { -31 } km/s and a core radius of 77 ^ { +10 } _ { -8 } kpc/h while an NFW profile has a a virial radius of 2.86 \pm 0.16 Mpc/h _ { 70 } and a concentration of 4.7 ^ { +0.6 } _ { -0.5 } .

The total mass profile is well described by either an NSIS profile with \sigma =1514 _ { -17 } ^ { +18 } km/s and core radius of r _ { c } =71 \pm 5 kpc/h _ { 70 } , or an NFW profile with C=6.0 \pm 0.5 and r _ { 200 } =2.82 \pm 0.11 Mpc/h _ { 70 } .
The errors are assumed to be due to the error in assigning masses to the individual galaxies in the galaxy component .
Their small size is due to the very strong constraints imposed by multiple images and the ability of the smooth dark matter component to adjust to uncertainties in the galaxy masses .
The derived total mass is in good agreement with the mass profile of despite the considerable differences in the methodology used .

Using also weak lensing shear measurements from we can constrain the profile further out to r \sim 2.5 Mpc/h _ { 70 } .
The best fit parameters change to \sigma =1499 \pm 15 km/s and r _ { c } =66 \pm 5 kpc/h _ { 70 } for the NSIS profile and C=7.6 \pm 0.5 and r _ { 200 } =2.55 \pm 0.07 Mpc/h _ { 70 } for the NFW profile .

Using the same image configuration as we obtain a strong lensing model that is superior to that of ( rms of 2.7 ” compared to 3.2 ” ) .
This is very surprising considering the larger freedom in the surface mass profile in their grid modelling .