We derive an accurate mass distribution of the galaxy cluster MACS J1206.2-0847 ( z = 0.439 ) from a combined weak-lensing distortion , magnification , and strong-lensing analysis of wide-field Subaru BVR _ { c } I _ { c } z ^ { \prime } imaging and our recent 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble ( CLASH ) program .
We find good agreement in the regions of overlap between several weak and strong lensing mass reconstructions using a wide variety of modeling methods , ensuring consistency .
The Subaru data reveal the presence of a surrounding large scale structure with the major axis running approximately north-west south-east ( NW-SE ) , aligned with the cluster and its brightest galaxy shapes , showing elongation with a \sim 2 : 1 axis ratio in the plane of the sky .
Our full-lensing mass profile exhibits a shallow profile slope d \ln \Sigma / d \ln R \sim - 1 at cluster outskirts ( R \lower 2.15 pt \hbox { $ \buildrel > \over { \sim } $ } 1 Mpc h ^ { -1 } ) , whereas the mass distribution excluding the NW-SE excess regions steepens further out , well described by the Navarro-Frenk-White form .
Assuming a spherical halo , we obtain a virial mass M _ { vir } = ( 1.1 \pm 0.2 \pm 0.1 ) \times 10 ^ { 15 } M _ { \odot } h ^ { -1 } and a halo concentration c _ { vir } = 6.9 \pm 1.0 \pm 1.2 ( c _ { vir } \sim 5.7 when the central 50 kpc h ^ { -1 } is excluded ) , which falls in the range 4 \lower 2.15 pt \hbox { $ \buildrel < \over { \sim } $ } \langle c \rangle \lower 2.15 pt% \hbox { $ \buildrel < \over { \sim } $ } 7 of average c ( M,z ) predictions for relaxed clusters from recent \Lambda cold dark matter simulations .
Our full lensing results are found to be in agreement with X-ray mass measurements where the data overlap , and when combined with Chandra gas mass measurements , yield a cumulative gas mass fraction of 13.7 ^ { +4.5 } _ { -3.0 } \% at 0.7 Mpc h ^ { -1 } ( \approx 1.7 r _ { 2500 } ) , a typical value observed for high mass clusters .