2009/08/31 by Keiichi Umetsu, Elinor Medezinski, Tom Broadhurst +4 · 3 citations
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Gravitational lens #Mass distribution #Space Technology and Applications #Subaru Telescope #Virial mass #Virial theorem #Weak gravitational lensing #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1088/0004-637x/714/2/1470
Accepted by ApJ; 35 pages, 25 figures; including gNFW fit results (Section 5.1), simulated post-shock temperatures consistent with X-ray results using T_{sl} (Section 7.3); Figures 7, 16, 24 added; a version with high resolution figures available at http://www.asiaa.sinica.edu.tw/~keiichi/upfiles/CL0024/ms_highreso.pdf
arxiv created 2010/03/25 · openalex publication_date 2010/04/20 · arxiv updated 2015/05/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 〉 ≃ 230 h ( M / L R ) ☉ , but exhibits a mild declining trend with increasing radius at cluster outskirts, r ≳ 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 ± 0.2) × 10 15 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 2–3 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 2D (< r vir ) = (1.4 ± 0.3) × 10 15 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.