Lens Models Under the Microscope: Comparison of Hubble Frontier Field Cluster Magnification Maps

TL;DR

This study compares multiple gravitational lensing models of galaxy clusters from the Hubble Frontier Fields, revealing significant discrepancies and uncertainties in magnification predictions, especially at high magnifications, due to lensing degeneracies.

Contribution

It provides a systematic comparison of different lens models for two galaxy clusters, highlighting the diversity and limitations of current mass reconstructions.

Findings

Model predictions vary by over 70% at high magnifications.

Different inversion techniques often produce results exceeding statistical errors.

Uncertainties are mainly due to lensing degeneracies, not just statistical errors.

Abstract

Using the power of gravitational lensing magnification by massive galaxy clusters, the Hubble Frontier Fields provide deep views of six patches of the high redshift Universe. The combination of deep Hubble imaging and exceptional lensing strength has revealed the greatest numbers of multiply-imaged galaxies available to constrain models of cluster mass distributions. However, even with $\mathcal{O}(100)$ images per cluster, the uncertainties associated with the reconstructions are not negligible. The goal of this paper is to show the diversity of model magnification predictions. We examine 7 and 9 mass models of Abell 2744 and MACS J0416, respectively, submitted to the Mikulski Archive for Space Telescopes for public distribution in September 2015. The dispersion between model predictions increases from 30% at common low magnifications ($\mu\sim2$) to 70% at rare high magnifications ($\mu\sim40$). MACS J0416 exhibits smaller dispersions than Abell 2744 for $2<\mu<10$. We show that magnification maps based on different lens inversion techniques typically differ from each other by more than their quoted statistical errors. This suggests that some models underestimate the true uncertainties, which are primarily due to various lensing degeneracies. Though the exact mass sheet degeneracy is broken, its generalized counterpart is not broken at least in Abell 2744. Other, local degeneracies are also present in both clusters. Our comparison of models is complementary to the comparison of reconstructions of known synthetic mass distributions. By focusing on observed clusters, we can identify those that are best constrained, and therefore provide the clearest view of the distant Universe.