arXiv 1510.034862015-10astro-ph.CO

MC ^2：利用哈勃望远镜和斯巴鲁弱透镜对“牙刷”星系团RX J0603 .3+4214暗物质分布的测绘

MC^2: Mapping the Dark Matter Distribution of the "Toothbrush" Cluster RX J0603.3+4214 with Hubble Space Telescope and Subaru Weak-lensing

M. James Jee, William A. Dawson, Andra Stroe, David Wittman, Reinout J. Van Weeren, Marcus Bruggen, Marusa Bradac, Huub Rottgering

备注：: Matched to the published version in ApJ
发表信息：: ApJ 817 (2016) 179
DOI：: 10.3847/0004-637X/817/2/179

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摘要：

z=0.225的星系团RX J0603.3+4214是最罕见的星系团之一，拥有非常大的射电遗迹（~2 Mpc）。由于遗迹的显著形态，该集群被昵称为“牙刷集群”。虽然星团的基本质量分布是重建令人费解的射电遗迹形态的合并场景所需的关键信息之一，但它接近银河平面b~10度的位置给观测带来了重大挑战。我们提出了一个高分辨率的弱透镜研究与斯巴鲁/Suprime凸轮和哈勃太空望远镜的成像数据的集群。我们的质量重建显示，该集群是由复杂的暗物质子结构密切跟踪星系的分布，但在相对简单的二元X射线形态形成对比。然而，我们发现星团质量仍然由南北方向排列的两个质量最大的星团占主导地位，其质量比约为3：1（北部和南部星团的M_{200} =6.29_{-1.62}^{+2.24} x 10^{14} Msun和1.98_{-0.74}^{+1.24} x 10^{14} Msun）。南部的质量峰相对于相应的X射线峰向南偏移约2'，其具有指向南方的“子弹”状形态。目前的弱透镜结果与X射线，星系和射电遗迹的比较表明，也许负责观测遗迹的主要机制可能是两个最大质量的子星系团的高速碰撞，尽管形态的特殊性需要额外的子星系团的参与。随后应进行仔细的数值模拟，以便利用所有现有的观测资料更全面地了解合并的情况。

英文摘要：

The galaxy cluster RX J0603.3+4214 at z=0.225 is one of the rarest clusters boasting an extremely large (~2 Mpc) radio-relic. Because of the remarkable morphology of the relic, the cluster is nicknamed "Toothbrush Cluster". Although the cluster's underlying mass distribution is one of the critical pieces of information needed to reconstruct the merger scenario responsible for the puzzling radio-relic morphology, its proximity to the Galactic plane b~10 deg has imposed significant observational challenges. We present a high-resolution weak-lensing study of the cluster with Subaru/Suprime Cam and Hubble Space Telescope imaging data. Our mass reconstruction reveals that the cluster is comprised of complicated dark matter substructures closely tracing the galaxy distribution, however in contrast with the relatively simple binary X-ray morphology. Nevertheless, we find that the cluster mass is still dominated by the two most massive clumps aligned north-south with a ~3:1 mass ratio (M_{200}=6.29_{-1.62}^{+2.24} x 10^{14} Msun and 1.98_{-0.74}^{+1.24} x 10^{14} Msun for the northern and southern clumps, respectively). The southern mass peak is ~2' offset toward the south with respect to the corresponding X-ray peak, which has a "bullet"-like morphology pointing south. Comparison of the current weak-lensing result with the X-ray, galaxy, and radio-relic suggests that perhaps the dominant mechanism responsible for the observed relic may be a high-speed collision of the two most massive subclusters, although the peculiarity of the morphology necessitates involvement of additional sub-clusters. Careful numerical simulations should follow in order to obtain more complete understanding of the merger scenario utilizing all existing observations.

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