The LISA Astrophysics MBHcatalogues Project: A comparison of predictions of simulated massive black hole binaries

TL;DR

This paper compares various theoretical models and simulations to predict massive black hole merger rates for LISA, analyzing uncertainties and dependencies on model assumptions.

Contribution

It provides a comprehensive comparison of 20 models and simulations to estimate MBH merger rates and their uncertainties for LISA observations.

Findings

Quantifies the spread in predicted MBH merger rates.

Evaluates the impact of model assumptions like seeding and simulation resolution.

Discusses how merger rates depend on astrophysical uncertainties.

Abstract

In the hierarchical paradigm of galaxy formation, central massive black holes (MBHs) are expected to coalesce after the merger of their host galaxies. One of the main goals of the Laser Interferometer Space Antenna (LISA) is to constrain the origin and growth of MBHs through their merger rates and mass distribution. Predicting MBH merger rates requires not only tracing their statistical population from large to small physical scales (kpc to sub-pc) but also modelling their formation, accretion, dynamics, mergers, and their galactic physical processes across cosmic time. This project is the result of a large collaborative effort undertaken by the LISA Astrophysics Working Group, bringing together its collective expertise on MBH formation, evolution, and modelling, to build a comprehensive understanding of MBH merger rates across cosmic time. The project compares various theoretical predictions of MBH merger rates, quantifies the spread, and evaluates the global astrophysical uncertainties of the LISA event rates. To build a unique and complete view, our work is based on about 20 semi-analytical models and cosmological simulations from the literature, all employing distinct approaches to modelling MBH and galaxy physics. To compute the merger rates, we also incorporate delays arising from the dynamical phase of MBH hardening to coalescence. We present the expected LISA merger rates given current galaxy formation models and discuss how the merger rate depends on model assumptions, such as the seeding model and the resolution of cosmological simulations.