Across the Universe: GW231123 as a magnified and diffracted black hole merger

TL;DR

This paper investigates GW231123, the most massive black hole merger observed, proposing that gravitational lensing, including diffraction by small objects, explains its observed properties and suggests it is magnified and distorted by a galaxy-scale lens.

Contribution

It introduces a novel analysis combining diffraction effects and gravitational magnification in lensing models of GW signals, providing new insights into the event's properties and lensing signatures.

Findings

Lensing is statistically favored with >99% confidence.

Including lensing reduces the estimated source mass to 100-180 M_4.

The event is likely magnified and possibly multiple images are formed.

Abstract

GW231123 appears as the most massive binary black hole (BBH) ever observed by the LIGO interferometers with total mass $190-265 M_\odot$. A high observed mass can be explained by the combination of cosmological redshift and gravitational magnification if the source is aligned with a gravitational lens, such as a galaxy. Small-scale objects such as stars and remnants diffract the signal, distorting the wavefront and providing additional lensing signatures. Here we present an analysis of GW231123 combining for the first time the effects of diffraction by a small-scale lens and gravitational magnification by an external potential, modelled as an embedded point-mass lens (PL), finding an intriguing case for the lensing hypothesis. Lensing is favoured by the data, with a false alarm probability of the observed Bayes factors bounded below $<1\%$, or $\sim 2.6 \sigma$ confidence level. Including lensing lowers the total source mass of GW231123 to $100-180 M_\odot$, closer to BBHs reported so far, and also removes discrepancies between different waveform approximants and the need for high component spins. We reconstruct all source and lens properties, including the microlens mass $190-850 M_\odot$, its offset, the magnitude of the external gravitational potential and its orientation. The embedded PL analysis leads to a lighter microlens compared to the isolated PL. Within our assumptions, the reconstruction is complete up to an ambiguity between the distance and projected density (mass-sheet degeneracy). Assuming a single galaxy as the macroscopic lens allows us to infer the total amplification of the signal, placing the event at redshift $0.7-2$, and predict the probability $~55\%$ of forming an additional detectable image due to strong lensing by the macrolens. We discuss the implications of our findings on the source and nature of the microlens, including a possible dark matter origin.