Ain't No Mountain High Enough: Semi-Parametric Modeling of LIGO-Virgos Binary Black Hole Mass Distribution

TL;DR

This paper presents a semi-parametric model for the primary mass distribution of binary black holes observed via gravitational waves, combining parametric and non-parametric methods to improve understanding of BBH formation.

Contribution

It introduces a cubic-spline perturbation approach to model BBH mass distribution, bridging parametric and non-parametric models for more accurate analysis.

Findings

Consistent with previous results showing a peak at 35 solar masses.

Potential signs of additional features at lower masses.

Simpler models remain compatible with current data.

Abstract

We introduce a semi-parametric model for the primary mass distribution of binary black holes (BBHs) observed with gravitational waves (GWs) that applies a cubic-spline perturbation to a power law. We apply this model to the 46 BBHs included in the second gravitational wave transient catalog (GWTC-2). The spline perturbation model recovers a consistent primary mass distribution with previous results, corroborating the existence of a peak at $35\,M_\odot$ ($>97\%$ credibility) found with the \textsc{Powerlaw+Peak} model. The peak could be the result pulsational pair-instability supernovae (PPISNe). The spline perturbation model finds potential signs of additional features in the primary mass distribution at lower masses similar to those previously reported by Tiwari and Fairhurst (2021). However, with fluctuations due to small number statistics, the simpler \textsc{Powerlaw+Peak} and \textsc{BrokenPowerlaw} models are both still perfectly consistent with observations. Our semi-parametric approach serves as a way to bridge the gap between parametric and non-parametric models to more accurately measure the BBH mass distribution. With larger catalogs we will be able to use this model to resolve possible additional features that could be used to perform cosmological measurements, and will build on our understanding of BBH formation, stellar evolution and nuclear astrophysics.