The Mass Density of Merging Binary Black Holes over Cosmic Time

Abstract

The connection between the binary black hole (BBH) mergers observed by LIGO-Virgo-KAGRA and their stellar progenitors remains uncertain. Specifically, the fraction ϵ of stellar mass that ends up in BBH mergers and the delay time τ between star formation and merger carry information about the astrophysical processes that produce merging BBHs. We model the merger rate in terms of cosmic star formation, coupled with a metallicity-dependent efficiency ϵ and a distribution of delay times τ , and infer these parameters with data from the Third Gravitational-Wave Transient Catalog. The progenitors to merging BBHs preferentially form in low-metallicity environments with a low-metallicity efficiency of ${\mathrm{log}}_{10}{\epsilon }_{\lt {Z}_{t}}=-{3.99}_{-0.87}^{+0.68}$ and a high-metallicity efficiency of ${\mathrm{log}}_{10}{\epsilon }_{\lt {Z}_{t}}=-{4.60}_{-0.34}^{+0.30}$ at 90% credibility. The data also prefer short delay times. For a power-law distribution p ( τ ) ∝ τ ^α , we find ${\tau }_{\min }\lt 1.9\,\mathrm{Gyr}$ and α 10 M _⊙ progenitors. However, because massive stars are short lived, there may be more mass in merging BBHs than in living massive stars as early as ∼2.5 Gyr ago. We also compare to the mass in supermassive black holes, finding that the densities were comparable ∼12.5 Gyr ago, but their densities quickly increased to ∼75 times the density in merging stellar-mass BBHs by z ∼ 1.

Keywords

• Gravitational waves
• Gravitational wave astronomy
• Black holes
• Binary stars
• Compact objects
• Stellar remnants