高分辨率 Magellan/Megacam 弱引力透镜揭示复杂并合后系统 A514 中的子结构内子结构
Substructures within Substructures in the Complex Post-Merging System A514 Unveiled by High-Resolution Magellan/Megacam Weak Lensing
AI总结：
研究利用高分辨率 Magellan/Megacam 弱透镜数据重建 A514 质量分布，发现 NW、SE 两个子星系团各自再分裂为双峰暗物质子结构，并据此推断其经历偏心碰撞。
摘要：
位于红移 z=0.071 的 Abell 514（A514）是一个引人关注的并合系统，表现出高度拉长（约 1 Mpc）的 X 射线特征以及三条大尺度（300～500 kpc）弯曲射电喷流。为利用其多波段数据剖析该系统，可靠地识别并量化其暗物质（DM）子结构至关重要。我们利用深度 Magellan/Megacam 观测对 A514 进行弱引力透镜分析。结合在最佳视宁度（约 0.″6）下获得的两个光学波段滤光片成像数据，并利用 A514 距离较近的优势，我们实现了约 46 arcmin^-2 或约 6940 Mpc^-2 的高源密度，从而能够进行高分辨率质量重建。我们揭示了 A514 复杂的暗物质子结构，其特征是相距约 0.7 Mpc 的 NW 和 SE 子星系团，且每个子星系团均呈现双峰质量分布。NW 子星系团的总质量估计为 M_200c^NW = 1.08_{-0.22}^{+0.24} × 10^14 M_⊙，并进一步分解为东部（M_200c^NW_E = 2.6_{-1.1}^{+1.4} × 10^13 M_⊙）和西部（M_200c^NW_W = 7.1_{-2.0}^{+2.3} × 10^13 M_⊙）成分。SE 子星系团的质量为 M_200c^SE = 1.55_{-0.26}^{+0.28} × 10^14 M_⊙，同样进一步分解为北部（M_200c^SE_N = 2.9_{-1.3}^{+1.8} × 10^13 M_⊙）和南部（M_200c^SE_S = 8.5_{-2.6}^{+3.0} × 10^13 M_⊙）成分。这四个子结构与 A514 的最亮星系位置重合，探测显著性为 3.4σ 至 4.8σ。暗物质子结构与 X 射线分布的比较表明，A514 可能经历过一次偏心碰撞，而 NW 和 SE 子星系团目前接近其远心点。
英文摘要：
Abell 514 (A514) at $z=0.071$ is an intriguing merging system exhibiting highly elongated (~1 Mpc) X-ray features and three large-scale (300~500 kpc) bent radio jets. To dissect this system with its multi-wavelength data, it is critical to robustly identify and quantify its dark matter (DM) substructures. We present a weak-lensing analysis of A514 using deep Magellan/Megacam observations. Combining two optical band filter imaging data obtained under optimal seeing (~0.''6) and leveraging the proximity of A514, we achieve a high source density of ~$46\mbox{arcmin}^{-2}$ or ~$\mathrm{6940Mpc^{-2}}$, which enables high-resolution mass reconstruction. We unveil the complex DM substructures of A514, which are characterized by the NW and SE subclusters separated by ~$0.7$Mpc, each exhibiting a bimodal mass distribution. The total mass of the NW subcluster is estimated to be $\mathrm{M^{NW}_{200c} = 1.08_{-0.22}^{+0.24} \times 10^{14} M_{\odot}}$ and is further resolved into the eastern ($\mathrm{M^{NW_E}_{200c} = 2.6_{-1.1}^{+1.4} \times 10^{13} M_{\odot}})$ and western ($\mathrm{M^{NW_W}_{200c} = 7.1_{-2.0}^{+2.3} \times 10^{13} M_{\odot}}$) components. The mass of the SE subcluster is $\mathrm{M^{SE}_{200c} = 1.55_{-0.26}^{+0.28} \times 10^{14} M_{\odot}}$, which is also further resolved into the northern ($\mathrm{M^{SE_N}_{200c} = 2.9_{-1.3}^{+1.8} \times 10^{13} M_{\odot}}$) and southern ($\mathrm{M^{SE_S}_{200c} = 8.5_{-2.6}^{+3.0} \times 10^{13} M_{\odot}}$) components. These four substructures coincide with the A514 brightest galaxies and are detected with significances ranging from 3.4$σ$ to 4.8$σ$. Comparison of the dark matter substructures with the X-ray distribution suggests that A514 might have experienced an off-axis collision, and the NW and SE subclusters are currently near their apocenters.
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