Hubble Space Telescope imaging of the galaxy cluster Abell 1689 has revealed an exceptional number of strongly lensed multiply-imaged galaxies, including high-redshift candidates. Previous studies have used this data to obtain the most detailed dark matter reconstructions of any galaxy cluster to date, resolving substructures ~25 kpc across. We examine Abell 1689 (hereafter, A1689) non-parametrically, combining strongly lensed images and weak distortions from wider field Subaru imaging, and we incorporate member galaxies to improve the lens solution. Strongly lensed galaxies are often locally affected by member galaxies, however, these perturbations cannot be recovered in grid based reconstructions because the lensing information is too sparse to resolve member galaxies. By adding luminosity-scaled member galaxy deflections to our smooth grid we can derive meaningful solutions with sufficient accuracy to permit the identification of our own strongly lensed images, so our model becomes self consistent. We identify 11 new multiply lensed system candidates and clarify previously ambiguous cases, in the deepest optical and NIR data to date from Hubble and Subaru. Our improved spatial resolution brings up new features not seen when the weak and strong lensing effects are used separately, including clumps and filamentary dark matter around the main halo. Our treatment means we can obtain an objective mass ratio between the cluster and galaxy components, for examining the extent of tidal stripping of the luminous member galaxies. We find a typical mass-to-light ratios of M/L_B = 21 inside the r<1 arcminute region that drops to M/L_B = 17 inside the r<40 arcsecond region. Our model independence means we can objectively evaluate the competitiveness of stacking cluster lenses for defining the geometric lensing-distance-redshift relation in a model independent way.
Constraining the masses of high-redshift clusters with weak lensing: Revised shape calibration testing for the impact of stronger shears and increased blending
Enabling Non-Parametric Strong Lensing Models to Derive Reliable Cluster Mass Distributions. WSLAP+
在强透镜制度的非参数透镜模型的斗争，以实现足够的角分辨率的中心集群质量分布的有意义的推导。问题主要在于集群成员扰动透镜图像并生成额外的图像，需要高分辨率建模，即使我们主要希望了解相对平滑的集群组件。所需的分辨率是无法实现的，因为透镜图像之间的间隔比成员星系的偏转角大几倍，即使是最深的数据。在这里，我们绕过这个限制，将一个简单的物理成员星系之前，使用它们的观测位置和光度标度质量。这个星系的贡献被添加到一个相对粗糙的高斯像素网格中，用于模拟星系团的质量分布，扩展了我们建立的WSDG代码（Diego et al. 2007）。我们测试这个新的代码与模拟的基础上A1689，使用的像素属于多透镜图像和观察到的成员星系。以这种方式处理集群成员会导致收敛的解决方案，而无需诉诸正则化，很好地再现了输入集群和子结构。我们强调这种方法的能力，以恢复黑暗的子组件的集群，无关的成员星系。这种异常现象可以提供线索的性质不可见的暗物质，但很难发现使用参数化模型的子结构是由可见的数据。随着我们的分辨率和稳定性的提高，我们第一次表明，非参数模型可以足够精确地定位多透镜系统，从而实现完全自洽的解决方案，而不依赖于输入系统从不太客观的手段。
Testing Offsets Between Cluster-Scale Halos and BCGs in Strong Lensing Models Using the Jackknife Method
Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理研究所）；Department of Astronomy, Yonsei University（延世大学天文学系）；Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France（艾克斯-马赛大学、法国国家科学研究中心、法国国家空间研究中心、拉格朗日实验室）；Department of Physics, University of California, Davis（加州大学戴维斯分校物理系）
CLASH: The Concentration-Mass Relation of Galaxy Clusters
通过对哈勃望远镜观测的19个星系团的X射线透镜分析，提出了一种新的星系团的浓度-质量关系的确定方法。我们的样本的红移范围在0.19到0.89之间。我们结合弱透镜约束从哈勃太空望远镜（HST）和地面宽场数据与强透镜约束从HST。其结果是重建的表面质量密度的所有CLASH集群的多尺度网格。我们对NFW参数的推导得到的维里质量在0.53 x 10^15和1.76 x 10^15 M_sol/h之间，晕浓度分布在c_200c ~ 3.7附近，与团簇质量呈1 σ显著负趋势。我们发现一个很好的4%之间的协议，我们的测量浓度和预期的数值模拟后占CLASH选择功能的基础上X射线形态。在2D中分析模拟，以考虑由于投影效应而导致的透镜重建中的可能偏差。理论浓度-质量（c-M）的关系，从我们的X射线选择的一组模拟集群和c-M关系直接从CLASH数据在90%的置信水平同意。
The Grism Lens-Amplified Survey from Space (GLASS). IV. Mass reconstruction of the lensing cluster Abell 2744 from frontier field imaging and GLASS spectroscopy
The Grism Lens-Amplified Survey from Space (GLASS). VI. Comparing the Mass and Light in MACSJ0416.1-2403 using Frontier Field imaging and GLASS spectroscopy
