Reconstructing the Lensing Mass in the Universe from Photometric Catalogue Data

TL;DR

This paper presents a method to reconstruct line-of-sight lensing effects using photometric data, improving the precision of cosmological distance measurements from gravitational lensing by about 50%.

Contribution

It introduces a halo model-based reconstruction technique for external convergence using mock catalogues, enhancing the accuracy of lensing-based cosmological inferences from photometric data.

Findings

Reconstruction improves precision of external convergence estimates by ~50%.

Selecting top third of lines of sight yields unbiased distance measurements with ~1% uncertainty.

Uncertainty in stellar mass-halo mass relation could bias results by ~2%.

Abstract

High precision cosmological distance measurements towards individual objects such as time delay gravitational lenses or type Ia supernovae are affected by weak lensing perturbations by galaxies and groups along the line of sight. In time delay gravitational lenses, "external convergence," kappa, can dominate the uncertainty in the inferred distances and hence cosmological parameters. In this paper we attempt to reconstruct kappa, due to line of sight structure, using a simple halo model. We use mock catalogues from the Millennium Simulation, and calibrate and compare our reconstructed P(kappa) to ray-traced kappa "truth" values; taking into account realistic observational uncertainties. We find that the reconstruction of kappa provides an improvement in precision of ~50% over galaxy number counts. We find that the lowest-kappa lines of sight have the best constrained P(kappa). In anticipation of large future samples of lenses, we find that selecting the third of the systems with the highest precision kappa estimates gives a sample of unbiased time delay distance measurements with just ~1% uncertainty due to line of sight external convergence effects. Photometric data are sufficient to pre-select the best-constrained lines of sight, and can be done before investment in light-curve monitoring. Conversely, we show that selecting lines of sight with high external shear could, with the reconstruction model presented, induce biases of up to 1% in time delay distance. We find that a major potential source of systematic error is uncertainty in the high mass end of the stellar mass-halo mass relation; this could introduce ~2% biases on the time-delay distance if completely ignored. We suggest areas for the improvement of this general analysis framework (including more sophisticated treatment of high mass structures) that should allow yet more accurate cosmological inferences to be made.