We derive an accurate mass distribution of the rich galaxy cluster Cl0024+1654 ( z = 0.395 ) based on deep Subaru BR _ { c } z ^ { \prime } imaging and our recent comprehensive strong lensing analysis of HST/ACS/NIC3 observations .
We obtain the weak lensing distortion and magnification of undiluted samples of red and blue background galaxies by carefully combining all color and positional information .
Unlike previous work , the weak and strong lensing are in excellent agreement where the data overlap .
The joint mass profile continuously steepens out to the virial radius with only a minor contribution \sim 10 \% in the mass from known subcluster at a projected distance of \simeq 700 kpc h ^ { -1 } .
The cluster light profile closely resembles the mass profile , and our model-independent M / L _ { R } profile shows an overall flat behavior with a mean of \langle M / L _ { R } \rangle \simeq 230 h ( M / L _ { R } ) _ { \odot } , but exhibits a mild declining trend with increasing radius at cluster outskirts , r \lower 2.15 pt \hbox { $ \buildrel > \over { \sim } $ } 0.6 r _ { vir } .
The projected mass distribution for the entire cluster is well fitted with a single Navarro-Frenk-White model with a virial mass , M _ { vir } = ( 1.2 \pm 0.2 ) \times 10 ^ { 15 } M _ { \odot } h ^ { -1 } , and a concentration , c _ { vir } = 9.2 ^ { +1.4 } _ { -1.2 } .
This model fit is fully consistent with the depletion of the red background counts , providing independent confirmation .
Careful examination and interpretation of X-ray and dynamical data , based on recent high-resolution cluster collision simulations , strongly suggest that this cluster system is in a post collision state , which we show is consistent with our well-defined mass profile for a major merger occurring along the line of sight , viewed approximately 2 - 3 Gyr after impact when the gravitational potential has had time to relax in the center , before the gas has recovered and before the outskirts are fully virialized .
Finally , our full lensing analysis provides a model-independent constraint of M _ { 2 D } ( < r _ { vir } ) = ( 1.4 \pm 0.3 ) \times 10 ^ { 15 } M _ { \odot } h ^ { -1 } for the projected mass of the whole system , including any currently unbound material beyond the virial radius , which can constrain the sum of the two pre-merger cluster masses when designing simulations to explore this system .