Analytic models of plausible gravitational lens potentials

TL;DR

This paper develops analytic models for gravitational lens potentials combining ellipsoidal symmetry, Sersic baryonic profiles, and truncated dark matter halos, enabling precise calculations of lensing effects and derivatives.

Contribution

It provides new analytic formulas for hybrid lens models with elliptical symmetry, truncated dark matter profiles, and higher-order derivatives, facilitating advanced lensing analyses.

Findings

Analytic expressions for lens potentials of Sersic profiles.

Formulas for truncated dark matter halo lensing effects.

Framework for modeling dark matter substructure and higher derivatives.

Abstract

Gravitational lenses on galaxy scales are plausibly modelled as having ellipsoidal symmetry and a universal dark matter density profile, with a Sersic profile to describe the distribution of baryonic matter. Predicting all lensing effects requires knowledge of the total lens potential: in this work we give analytic forms for that of the above hybrid model. Emphasising that complex lens potentials can be constructed from simpler components in linear combination, we provide a recipe for attaining elliptical symmetry in either projected mass or lens potential. We also provide analytic formulae for the lens potentials of Sersic profiles for integer and half-integer index. We then present formulae describing the gravitational lensing effects due to smoothly-truncated universal density profiles in cold dark matter model. For our isolated haloes the density profile falls off as radius to the minus fifth or seventh power beyond the tidal radius, functional forms that allow all orders of lens potential derivatives to be calculated analytically, while ensuring a non-divergent total mass. We show how the observables predicted by this profile differ from that of the original infinite-mass NFW profile. Expressions for the gravitational flexion are highlighted. We show how decreasing the tidal radius allows stripped haloes to be modelled, providing a framework for a fuller investigation of dark matter substructure in galaxies and clusters. Finally we remark on the need for finite mass halo profiles when doing cosmological ray-tracing simulations, and the need for readily-calculable higher order derivatives of the lens potential when studying catastrophes in strong lenses.