WEAK-LENSING MASS MEASUREMENTS OF SUBSTRUCTURES IN COMA CLUSTER WITH SUBARU/SUPRIME-CAM
WEAK-LENSING MASS MEASUREMENTS OF SUBSTRUCTURES IN COMA CLUSTER WITH SUBARU/SUPRIME-CAM
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DOI：
10.1088/0004-637x/713/1/291
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发表时间：
2010-01
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通讯作者：
N. Okabe;Y. Okura;Toshifumi Futamase Academia Sinica Institute of Astronomy-Toshifumi-Futamase-Academia-Sinica-Institute-of-102346417;Astrophysics;A. Institute;T. University;National Space Development Agency of Japan
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作者：
N. Okabe;Y. Okura;Toshifumi Futamase Academia Sinica Institute of Astronomy-Toshifumi-Futamase-Academia-Sinica-Institute-of-102346417;Astrophysics;A. Institute;T. University;National Space Development Agency of Japan
通过弱透镜分析，我们得到了后发座星系团（z = 0.0236）西南区（r = 60′）的两个Subaru/Suprime-Cam场的投影质量分布，并探测到了8个候选子星系团.我们量化的贡献，背景大尺度结构（LSS）的投影质量分布使用斯隆数字巡天多波段和光度数据，场星系的质光比的假设下。我们发现，八个子团候选人，这是不与任何成员星系，是显着的LSS透镜的影响。从主星系团势中提取出的7个子团的平均投影质量为：LSS修正后的2D τ =（5.06 ± 1.30）× 1012 h−1 M τ。一个切向畸变剖面上的子块系综被截断的奇异等温球模型和截断Navarro-Frenk-白色模型很好地描述。子团的典型截断半径rt <$35 h−1 kpc，是在没有假设成员星系的质量和光之间有任何关系的情况下推导出来的。这个半径与主星团引力的潮汐半径（1042 h−1 kpc）非常吻合。考虑到数据区域的不完整性、投影效应和虚假透镜峰，预计团簇子结构的质量占维里质量的19%，统计误差为13%。团簇子结构的质量分数与数值模拟结果基本一致。
We obtain the projected mass distributions for two Subaru/Suprime-Cam fields in the southwest region (r ≲ 60′) of the Coma Cluster (z = 0.0236) by weak-lensing analysis and we detect eight subclump candidates. We quantify the contribution of background large-scale structure (LSS) on the projected mass distributions using Sloan Digital Sky Survey multi-bands and photometric data, under the assumption of mass-to-light ratio for field galaxies. We find that one of the eight subclump candidates, which is not associated with any member galaxies, is significantly affected by LSS lensing. The mean projected mass for the seven subclumps extracted from the main cluster potential is 〈M(corr)2D〉 = (5.06 ± 1.30) × 1012 h−1 M☉ after an LSS correction. A tangential distortion profile over an ensemble of subclumps is well described by a truncated singular-isothermal sphere model and a truncated Navarro–Frenk–White model. A typical truncated radius of subclumps, rt ≃ 35 h−1 kpc, is derived without assuming any relations between mass and light for member galaxies. The radius coincides well with the tidal radius, ∼42 h−1 kpc, of the gravitational force of the main cluster. Taking into account the incompleteness of the data area, a projection effect, and spurious lensing peaks, it is expected that the mass of the cluster substructures accounts for 19% of the virial mass, with 13% statistical error. The mass fraction of the cluster substructures is in rough agreement with numerical simulations.