STRIDES: automated uniform models for 30 quadruply imaged quasars
STRIDES: automated uniform models for 30 quadruply imaged quasars
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STRIDES：30 个四重成像类星体的自动化统一模型
DOI：
10.1093/mnras/stac2235
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发表时间：
2022
影响因子：
4.8
通讯作者：
Auger-Williams, M W
中科院分区：
文献类型：
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作者：
Schmidt, T;Treu, T;Birrer, S;Shajib, A J;Lemon, C;Millon, M;Sluse, D;Agnello, A;Anguita, T;Auger-Williams, M W
引力时间延迟提供了一个强大的一步测量H 0，独立于所有其他探头。延时宇宙学的一个关键要素是高精度的透镜模型。就计算和调查时间而言，目前获得这些数据的成本很高（分别为105- 106 CPU小时和10.5 -1年）。因此，建模速度的重大改进是必要的，以利用预测将在本十年内发现的大量透镜。为了绕过这一障碍，我们开发了一个自动建模管道，并将其应用于31个透镜系统的样本，由哈勃太空望远镜在多个波段观察。我们的自动化流水线可以用几个小时的人工时间和<100个CPU小时的计算时间为典型系统导出30/31镜头的模型。对于每个透镜，我们提供了关键参数的测量和放大率的预测，以及多个图像的时间延迟。我们使用费马势（与时间延迟成比例）的差异相对于建模选择的稳定性来表征我们的模型的宇宙学准备。我们发现，对于10/30镜片，我们的模型是宇宙学级或接近宇宙学级（<3%和3- 5%的变化）。对于6/30镜片，模型接近宇宙学等级（5- 10%）。这些结果利用信息先验，并将需要通过进一步的分析来确认。然而，它们也有可能通过扩展管道建模序列和选项来改进。总之，我们表明，大型强透镜样品的统一宇宙学等级建模是触手可及的。
Gravitational time delays provide a powerful one-step measurement ofH0, independent of all other probes. One key ingredient in time-delay cosmography are high-accuracy lens models. Those are currently expensive to obtain, both, in terms of computing and investigator time (105–106CPU hours and ∼0.5–1 yr, respectively). Major improvements in modelling speed are therefore necessary to exploit the large number of lenses that are forecast to be discovered over the current decade. In order to bypass this roadblock, we develop an automated modelling pipeline and apply it to a sample of 31 lens systems, observed by theHubble Space Telescopein multiple bands. Our automated pipeline can derive models for 30/31 lenses with few hours of human time and <100 CPU hours of computing time for a typical system. For each lens, we provide measurements of key parameters and predictions of magnification as well as time delays for the multiple images. We characterize the cosmography-readiness of our models using the stability of differences in the Fermat potential (proportional to time delay) with respect to modelling choices. We find that for 10/30 lenses, our models are cosmography or nearly cosmography grade (<3 per cent and 3–5 per cent variations). For 6/30 lenses, the models are close to cosmography grade (5–10 per cent). These results utilize informative priors and will need to be confirmed by further analysis. However, they are also likely to improve by extending the pipeline modelling sequence and options. In conclusion, we show that uniform cosmography grade modelling of large strong lens samples is within reach.