The strongest gravitational lenses: III. The order statistics of the largest Einstein radii
The strongest gravitational lenses: III. The order statistics of the largest Einstein radii
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最强引力透镜：III。
DOI：
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发表时间：
2014
期刊：
影响因子：
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通讯作者：
M. Bartelmann
中科院分区：
文献类型：
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作者：
Jean;Matthias Redlich;M. Meneghetti;M. Bartelmann
上下文引力透镜的爱因斯坦半径是一个关键特性。它编码的信息决定性的数量，如晕质量，浓度，三轴度，相对于观察者的方向。因此，最大的爱因斯坦半径可能被用来测试ΛCDM模型的预测。目标。目前，研究主要集中在单个最大的爱因斯坦半径上。我们扩展了这些研究，采用顺序统计，制定排除标准的基础上的n个最大的爱因斯坦半径和应用这些标准的强透镜分析的12个MACS集群在z > 0.5。方法.我们得到的顺序统计量的爱因斯坦半径的Monte Carlo方法，基于过去的光锥上的晕人口的半解析建模。在对顺序统计量进行采样之后，我们将一般极值分布拟合到一阶分布，这使我们能够推导出爱因斯坦半径的顺序统计量的解析关系。结果我们发现12个MACS星系团的Einstein半径与ΛCDM理论的期望值并不冲突。我们的排除标准表明，为了展示和谐模型的张力，在红移范围0.5 ≤ z ≤ 1内，需要观察到大约20个θ eff> 30 Ω的爱因斯坦半径，10个θeff > 35 Ω的爱因斯坦半径，5个θeff > 42 Ω的爱因斯坦半径，或者1个θeff > 74 Ω的爱因斯坦半径。在整个天空中（假设源红移zs = 2）。此外，我们发现，随着增加的顺序，最大的爱因斯坦半径的晕是平均较少的沿着视线和较少的三轴对齐。一般来说，累积分布函数在高阶时变陡，使它们具有更好的约束能力。结论.一个框架，允许个人和联合的顺序分布的n-最大的爱因斯坦半径推导。从统计的角度来看，我们没有看到任何证据的爱因斯坦环问题，即使是最大的爱因斯坦半径的研究MACS样本。这个结论是巩固了大的不确定性，进入透镜模型和最大的爱因斯坦半径是特别敏感。
Context. The Einstein radius of a gravitational lens is a key characteristic. It encodes information about decisive quantities such as halo mass, concentration, triaxiality, and orientation with respect to the observer. Therefore, the largest Einstein radii can potentially be utilised to test the predictions of the ΛCDM model. Aims. Hitherto, studies have focussed on the single largest observed Einstein radius. We extend those studies by employing order statistics to formulate exclusion criteria based on the n largest Einstein radii and apply these criteria to the strong lensing analysis of 12 MACS clusters at z > 0.5. Methods. We obtain the order statistics of Einstein radii by a Monte Carlo approach, based on the semi-analytic modelling of the halo population on the past lightcone. After sampling the order statistics, we fit a general extreme value distribution to the first-order distribution, which allows us to derive analytic relations for the order statistics of the Einstein radii. Results. We find that the Einstein radii of the 12 MACS clusters are not in conflict with the ΛCDM expectations. Our exclusion criteria indicate that, in order to exhibit tension with the concordance model, one would need to observe approximately twenty Einstein radii with θeff > 30 �� , ten with θeff > 35 �� , five with θeff > 42 �� , or one with θeff > 74 �� in the redshift range 0.5 ≤ z ≤ 1. 0o n the full sky (assuming a source redshift of zs = 2). Furthermore, we find that, with increasing order, the haloes with the largest Einstein radii are on average less aligned along the line-of-sight and less triaxial. In general, the cumulative distribution functions steepen for higher orders, giving them better constraining power. Conclusions. A framework that allows the individual and joint order distributions of the n-largest Einstein radii to be derived is presented. From a statistical point of view, we do not see any evidence of an Einstein ring problem even for the largest Einstein radii of the studied MACS sample. This conclusion is consolidated by the large uncertainties that enter the lens modelling and to which the largest Einstein radii are particularly sensitive.
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.
最强引力透镜 - II MACS J0717 5 3745 的大爱因斯坦半径与 ÎCDM 冲突吗？
影响因子：
6.5
作者：
J.-C. Waizmann;M. Redlich;M. Bartelmann
通讯作者：
M. Bartelmann