High-Spin BBH Subpopulation from AGN Accretion

TL;DR

This study identifies a subpopulation of black hole mergers with high spins consistent with accretion in AGN disks, providing population-level evidence for this formation channel.

Contribution

It offers the first observational evidence of an accretion-origin subpopulation in black hole mergers using spin data and mixture modeling.

Findings

Approximately 10% of detected mergers belong to the high-spin accretion subpopulation.

High-spin subpopulation has primary spins near 0.9, matching accretion predictions.

Accretion candidates tend to have higher masses and aligned spins.

Abstract

The formation environments of merging binary black holes remain uncertain. While hierarchical assembly in dense stellar clusters has been widely explored as an explanation for black holes exceeding the stellar-mass limit, growth through gas accretion in active galactic nucleus (AGN) disks is an alternative that has received less observational scrutiny. Here we search for an accretion-origin subpopulation using only spin magnitudes, fitting a three-component mixture model to 166 binary black hole mergers from LIGO--Virgo--KAGRA with component shapes fixed from theoretical predictions and only the mixing fractions inferred from the data. We find strong evidence ($ln B = 5.7$) that $\sim 10\%$ (90% credible interval $[1\%, 14\%]$) of detected mergers belong to a subpopulation with primary spins clustered near $a_1 \approx 0.9$, consistent with the theoretical prediction for accretion spin-up. The hierarchical-merger prediction of $a_1 \approx 0.7$ is decisively disfavored as the location of the high-spin subpopulation ($ln B = 5.7$). Post hoc validation reveals that the accretion candidates have systematically higher masses (median $m_1 = 58\,M_\odot$) and aligned spins (median $\chi_{\rm eff} = 0.33$, vs. $0.04$ for standard-dominated events). The accretion subpopulation is not limited to systems above the pair-instability mass gap: GW190517 ($m_1 \approx 39 M_\odot$) is among the top candidates, demonstrating that accretion spin-up operates across a range of masses. GW190521, previously interpreted as a hierarchical merger, shows comparable support for an accretion origin. These results provide the first population-level observational evidence for an accretion-origin subpopulation in black hole mergers.