标题： 一种对28个强引力透镜区域的光谱调查：对$H_0$的意义 显示英文标题

标题： A Spectroscopic Survey of the Fields of 28 Strong Gravitational Lenses: Implications for $H_0$

摘要： 强引力透镜为哈勃参数（$H_0$）提供了独立的测量方法。 一个剩余的系统性偏差是由于透镜红移处或视线方向的星系团额外质量引起的偏差。 我们对超过20个具有良好采样视线质量分布的强透镜量化了这种偏差，重点关注会聚度$\kappa$和剪切力$\gamma$。 在这些区域的23%中，透镜星系团导致了$\ge$1%的会聚偏差；在57%的区域中，存在同样显著的视线星系团。 对于九个时间延迟透镜系统，当忽略星系团时，$H_0$平均被高估了11$^{+3}_{-2}$%。 在总$\kappa \ge$为 0.01 的 67% 的区域中，视线组比透镜组贡献了$\gtrsim 2\times$更多的汇聚，这表明透镜组并不是唯一的重要的质量。 透镜环境影响四像（quad）与二像（double）系统之间的比率；所有七个四像都有透镜组，而 10 个二像中只有三个有透镜组，由透镜组引起的最高汇聚出现在四像中。 我们校准$\gamma$-$\kappa$关系：$\log(\kappa_{\rm{tot}}) = (1.94 \pm 0.34) \log(\gamma_{\rm{tot}}) + (1.31 \pm 0.49)$，均方根散度为 0.34 次方。 剪切，与收敛不同，可以从透镜图像中直接测量，但可能是$\kappa$的不良预测因子；在我们 19% 的区域中，$\kappa$是$\gtrsim 2\gamma$。因此，使用强引力透镜进行精确宇宙学需要对每个透镜场中的所有显著结构进行精确测量和校正。 显示英文摘要

摘要： Strong gravitational lensing provides an independent measurement of the Hubble parameter ($H_0$). One remaining systematic is a bias from the additional mass due to a galaxy group at the lens redshift or along the sightline. We quantify this bias for more than 20 strong lenses that have well-sampled sightline mass distributions, focusing on the convergence $\kappa$ and shear $\gamma$. In 23% of these fields, a lens group contributes a $\ge$1% convergence bias; in 57%, there is a similarly significant line-of-sight group. For the nine time delay lens systems, $H_0$ is overestimated by 11$^{+3}_{-2}$% on average when groups are ignored. In 67% of fields with total $\kappa \ge$ 0.01, line-of-sight groups contribute $\gtrsim 2\times$ more convergence than do lens groups, indicating that the lens group is not the only important mass. Lens environment affects the ratio of four (quad) to two (double) image systems; all seven quads have lens groups while only three of 10 doubles do, and the highest convergences due to lens groups are in quads. We calibrate the $\gamma$-$\kappa$ relation: $\log(\kappa_{\rm{tot}}) = (1.94 \pm 0.34) \log(\gamma_{\rm{tot}}) + (1.31 \pm 0.49)$ with a rms scatter of 0.34 dex. Shear, which, unlike convergence, can be measured directly from lensed images, can be a poor predictor of $\kappa$; for 19% of our fields, $\kappa$ is $\gtrsim 2\gamma$. Thus, accurate cosmology using strong gravitational lenses requires precise measurement and correction for all significant structures in each lens field.