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

TL;DR

This study quantifies the impact of galaxy groups along sightlines on Hubble constant measurements from strong gravitational lensing, highlighting the importance of accounting for line-of-sight structures to reduce bias.

Contribution

It provides a detailed analysis of mass contributions from lens and line-of-sight groups, calibrates the shear-convergence relation, and emphasizes the need for precise measurements for accurate cosmology.

Findings

Line-of-sight groups cause significant convergence bias in 57% of fields.

Ignoring groups leads to an 11% overestimation of H0 in time delay lenses.

Shear can be a poor predictor of convergence, with 19% of fields showing high convergence relative to shear.

Abstract

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.