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' imaging and our recent 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble 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 northwest-southeast (NW-SE), aligned with the cluster and its brightest galaxy shapes, showing elongation with a ~2: 1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope dln Σ/dln R ~ –1 at cluster outskirts (R 1?Mpc?h –1), whereas the mass distribution excluding the NW-SE excess regions steepens farther out, well described by the Navarro-Frenk-White form. Assuming a spherical halo, we obtain a virial mass M vir = (1.1 ± 0.2 ± 0.1) × 1015 M ☉ h –1 and a halo concentration c vir = 6.9 ± 1.0 ± 1.2 (c vir ~ 5.7 when the central 50?kpc?h –1 is excluded), which falls in the range 4 c 7 of average c(M, z) predictions for relaxed clusters from recent Λ 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, they yield a cumulative gas mass fraction of 13.7+4.5 – 3.0% at 0.7?Mpc?h –1(≈ 1.7 r 2500), a typical value observed for high-mass clusters.
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机译：我们通过对广角斯巴鲁BVR c I cz'成像的弱透镜畸变，放大倍率和强透镜分析的综合以及我们的结合得出银河团MACS？J1206.2-0847（z = 0.439）的精确质量分布最近的16波段哈勃太空望远镜观测结果，是哈勃计划进行的星团透镜和超新星调查的一部分。我们使用多种建模方法在几次弱镜头和强镜头大规模重建的重叠区域中找到了很好的一致性，从而确保了一致性。斯巴鲁（Subaru）的数据揭示了周围存在的大型结构，其主轴线大约在西北偏南（NW-SE）方向，与星团及其最明亮的星系形状对齐，显示出伸长率为〜2：1的轴比。天空的飞机。我们的全透镜质量轮廓在簇状郊区（R 1？Mpc？h –1）处表现出较浅的轮廓斜率dlnΣ/ dln R〜–1，而不包括NW-SE多余区域的质量分布更陡峭，很好地描述了由Navarro-Frenk-White形式。假设球形光晕，我们得到病毒质量M vir =（1.1±0.2±0.1）×1015 M☉h –1，光晕浓度c vir = 6.9±1.0±1.2（当中心50？kpc时c vir〜5.7 ？h –1排除在外），其范围在最近Λ冷暗物质模拟得出的松弛星团的平均c（M，z）预测的4 c 7范围内。我们的全透镜结果与数据重叠的X射线质量测量结果吻合，并且与钱德拉气体质量测量结果结合使用时，它们在0.7？Mpc？的累积气体质量分数为13.7 + 4.5 – 3.0％。 h –1（≈1.7 r 2500），这是对高质量星团观察到的典型值。
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