A Spectroscopic Redshift for the Cl 0024+16 Multiple Arc System: Implications for the Central Mass Distribution
A Spectroscopic Redshift for the Cl 0024+16 Multiple Arc System: Implications for the Central Mass Distribution
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Cl 0024 16 多弧系统的光谱红移：对中心质量分布的影响
DOI：
10.1086/312651
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发表时间：
1999
期刊：
影响因子：
--
通讯作者：
R. Ellis
中科院分区：
文献类型：
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作者：
T. Broadhurst;Xiaosheng Huang;B. Frye;R. Ellis
我们提出了在z = 0.39的星团Cl 0024+16中看到的著名的多透镜弧系统的光谱红移为z = 1.675。与早期的工作相反，我们发现透镜图像可以通过一个投影质量分布精确地再现，该分布追踪了最亮的星团椭圆星系的位置，这表明星团势的最显著最小值并没有被动态地抹去。平均质量剖面较浅，与最近数值模拟的预测一致。源红移使我们能够确定一个封闭星团的质量M(<100 kpc h-1) = 1.11±0.03 × 1014 h-1 M☉（Ω = 1）和质量光比M/LB(<100 kpc h-1) = 320±30 h （M/LB）☉（实际上与曲率无关），经过被动恒星演化的校正。弧线光谱包含许多电离吸收线，与当地的沃尔夫-拉叶星系NGC 4217非常相似。我们的透镜模型预测每个图像的高放大率（≃20），并在预测的红移z = 1.3时识别出一个星系的一对新的多重图像。
We present a spectroscopic redshift of z = 1.675 for the well-known multiply lensed system of arcs seen in the z = 0.39 cluster Cl 0024+16. In contrast to earlier work, we find that the lensed images are accurately reproduced by a projected mass distribution which traces the locations of the brightest cluster elliptical galaxies, suggesting that the most significant minima of the cluster potential are not dynamically erased. The averaged mass profile is shallow and consistent with predictions of recent numerical simulations. The source redshift enables us to determine an enclosed cluster mass of M(<100 kpc h-1) = 1.11 ± 0.03 × 1014 h-1 M☉ (Ω = 1) and a mass-to-light ratio of M/LB(<100 kpc h-1) = 320 ± 30 h (M/LB)☉ (virtually independent of curvature), after correction for passive stellar evolution. The arc spectrum contains many ionized absorption lines and closely resembles that of the local Wolf-Rayet galaxy NGC 4217. Our lens model predicts a high magnification (≃20) for each image and identifies a new pair of multiple images of a galaxy at a predicted redshift of z = 1.3.