论文标题
第一个倍数成像的超新星的课程：Galaxy群集Mac的修订的光跟踪强镜头模型J1149.5+2223
Lessons from the first multiply imaged supernova: A revised Light-Traces-Mass strong lensing model for the galaxy cluster MACS J1149.5+2223
论文作者
论文摘要
我们的MAC的光跟踪质量（LTM）强镜模型J1149.5+2223在过去十年中扮演了多个关键角色：它有助于在此群集中识别多个图像的识别以及对Redshift $ Z \ simeq9 $的MAC1149-JD1的研究晶状体镜头1。SupernovaRefsdal提供了一个无价的机会，以盲目测试通用镜头模型技术的能力，以准确描述SN Refsdal图像的属性并预测其柜台图像之一的重新出现，这是由于原始Einserstein的原始eInserstein的一年。由于这种做法，我们提交的模型产生了一些外围结果，我们在代码的时间延迟（TD）计算部分中找到了数值伪像，该部分现在已修复。该伪影不影响多个图像的再现（即偏转场 - 直接受到观察结果的约束）或派生的质量模型，因此在超新星参考文献之前，它一直没有引起人们的注意，强调了盲人测试在天文学中的重要性。在这里，我们更新了模型，并为Refsdal提供了修订后的LTM测量。这些不仅对于完成REFSDAL事件的LTM视图很重要，还因为它们会影响不同镜头模型技术预测的值范围，因此会影响TD计算的系统不确定性范围和结果的哈勃常数。
Our light-traces-mass (LTM) strong-lensing model for MACS J1149.5+2223 has played several key roles over the last decade: it aided the identification of multiple images in this cluster and the study of MACS1149-JD1 at redshift $z\simeq9$, it was used to estimate the properties of the first multiply imaged supernova, Refsdal, in its discovery paper, and of the first caustic crossing event by a cluster, Lensed Star 1. Supernova Refsdal supplied an invaluable opportunity to conduct a blind test of the ability of common lens-modeling techniques to accurately describe the properties of SN Refsdal's images and predict the reappearance of one of its counter images that was due about a year post-discovery of the original Einstein cross. Thanks to this practice, in which our submitted model yielded some outlying results, we located a numerical artifact in the time delay (TD) calculation part of the code, which was now fixed. This artifact did not influence the reproduction of multiple images (i.e., the deflection fields -- which are those constrained directly from the observations) or the derived mass model, and so it remained unnoticed prior to supernova Refsdal, emphasizing the importance of blind tests in astronomy. Here we update our model and present revised LTM measurements for Refsdal. These are important not only for completing the LTM view of the Refsdal event, but also because they affect the range of values predicted from different lens-modeling techniques and thus the range of systematic uncertainties for the TD calculation and the resulting Hubble constant.
