An upper limit on the spins of merging binary black holes formed through isolated binary evolution

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Volume 691 (November 2024)

A&A, 691 (2024) A339

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Table 2.

Predicted detection rates (per year of detector time) for BBH mergers produced from CHE, derived from the simulations of dB20.

		χ_eff < 0.5,	χ_eff > 0.5,	χ_eff < 0.5,	χ_eff > 0.5,
Detector	Full	$\frac{M_{chirp}}{M_{⊙}} < 30$ $\displaystyle\frac{M_{\mathrm{chirp}}}{\mathrm{M}_\odot} < 30$	$\frac{M_{chirp}}{M_{⊙}} < 30$ $\displaystyle\frac{M_{\mathrm{chirp}}}{\mathrm{M}_\odot} < 30$	$30 < \frac{M_{chirp}}{M_{⊙}} < 38.3$ $\displaystyle30 < \frac{M_{\mathrm{chirp}}}{\mathrm{M}_\odot} < 38.3$	$30 < \frac{M_{chirp}}{M_{⊙}} < 38.3$ $\displaystyle30 < \frac{M_{\mathrm{chirp}}}{\mathrm{M}_\odot} < 38.3$	$\frac{M_{chirp}}{M_{⊙}} > 107$ $\displaystyle\frac{M_{\mathrm{chirp}}}{\mathrm{M}_\odot} > 107$
Cosmological	8600	1200	2800	1500	1300	1900
O3	80	31	13	20	7.5	7.3
O4	290	100	61	68	33	30
O5/A+	1700	420	550	320	260	170

Notes. Row marked as “Cosmological” represents the full rate observable from Earth with a detector of infinite sensitivity. Column marked “Full” shows the full rate for each detector, while the other columns represent subsets of the full population filtered by their effective spins and masses.

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