Generalised model-independent characterisation of strong gravitational lenses I: Theoretical foundations

TL;DR

This paper generalizes a model-independent method for characterizing strong gravitational lenses, enabling more flexible analysis of multiple image configurations and improving accuracy in determining lens properties.

Contribution

It extends the previous approach to its most general form by incorporating orientation angles and removing symmetry assumptions, enhancing the analysis of complex lensing scenarios.

Findings

Position of critical points reconstructed with less than 5" deviation.

Critical curve slope and shape deviate less than 20% near critical points.

Approach applicable to galaxy cluster scale lensing with high accuracy.

Abstract

We extend the model-independent approach to characterise strong gravitational lenses of Wagner & Bartelmann (2016) to its most general form to leading order by using the orientation angles of a set of multiple images with respect to their connection line(s) in addition to the relative distances between the images, their ellipticities and time-delays. For two symmetric images that straddle the critical curve, the orientation angle additionally allows to determine the slope of the critical curve and a second (reduced) flexion coefficient at the critical point on the connection line between the images. It also allows to drop the symmetry assumption that the axis of largest image extension is orthogonal to the critical curve. For three images almost forming a giant arc, the degree of assumed image symmetry is also reduced to the most general case, allowing to describe image configurations for which the source need not be placed on the symmetry axis of the two folds that unite at the cusp. For a given set of multiple images, we set limits on the applicability of our approach, show which information can be obtained in cases of merging images, and analyse the accuracy achievable due to the Taylor expansion of the lensing potential for the fold case on a galaxy cluster scale NFW-profile, a fold and cusp case on a galaxy cluster scale SIE-profile, and compare the generalised approach with the one of Wagner & Bartelmann (2016). The position of the critical points is reconstructed with less than 5" deviation for multiple images closer to the critical points than 30\% of the (effective) Einstein radius and the slope of the critical curve at a fold and its shape in the vicinity of a cusp deviate less than 20\% from the true values for distances of the images to the critical points less than 15\% of the (effective) Einstein radius.