The mass structure of the galaxy cluster Cl0024+1654 from a full lensing analysis of joint subaru and ACS/NIC3 observations

We derive an accurate mass distribution of the rich galaxy cluster Cl0024+1654 (z = 0.395) based on deep Subaru BR _c z′ imaging and our recent comprehensive strong-lensing analysis of Hubble Space Telescope/Advanced Camera for Surveys/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 10% in the mass from known subcluster at a projected distance of ≃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 〈M/L_R 〉 ≃ 230h(M/L_R )_⊙, but exhibits a mild declining trend with increasing radius at cluster outskirts, r ≳ 0.6r _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 ± 0.2) × 10¹⁵ M _⊙ 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 2-3Gyr 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 _2D(<r _vir) = (1.4 ± 0.3) × 10¹⁵ M _⊙ 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.