Compactness peaks: An astrophysical interpretation of the mass distribution of merging binary black holes

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Volume 694 (February 2025)

A&A, 694 (2025) A186

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Table 1.

Properties of events ‘polluting’ the component-mass gap (m = 10 − 15 M_⊙).

Event; [REF]	q	χ_eff	χ_p	Suggestions for other formation scenarios
GW190412_053044; [1]	$0 . 28_{- 0.06}^{+ 0.12}$ $0.28^{+0.12}_{-0.06}$	$0 . 25_{- 0.11}^{+ 0.08}$ $0.25^{+0.08}_{-0.11}$	$0 . 31_{- 0.16}^{+ 0.2}$ $0.31^{+0.2}_{-0.16}$	e.g. Safarzadeh & Hotokezaka (2020), Gerosa et al. (2020), Liu & Lai (2021)
GW151226; [2]	$0 . 57_{- 0.34}^{+ 0.37}$ $0.57^{+0.37}_{-0.34}$	$0 . 18_{- 0.12}^{+ 0.2}$ $0.18^{+0.2}_{-0.12}$	$0 . 5_{- 0.33}^{+ 0.39}$ $0.5^{+0.39}_{-0.33}$	e.g. Chatterjee et al. (2017)
GW190828_065509; [3]	$0 . 43_{- 0.16}^{+ 0.38}$ $0.43^{+0.38}_{-0.16}$	$0 . 08_{- 0.16}^{+ 0.15}$ $0.08^{+0.15}_{-0.16}$	$0 . 29_{- 0.21}^{+ 0.41}$ $0.29^{+0.41}_{-0.21}$	–
GW200316_215756; [4]	$0 . 6_{- 0.39}^{+ 0.34}$ $0.6^{+0.34}_{-0.39}$	$0 . 12_{- 0.1}^{+ 0.28}$ $0.12^{+0.28}_{-0.1}$	$0 . 29_{- 0.21}^{+ 0.4}$ $0.29^{+0.4}_{-0.21}$	–
GW190728_064510; [3]	$0 . 68_{- 0.31}^{+ 0.27}$ $0.68^{+0.27}_{-0.31}$	$0 . 12_{- 0.06}^{+ 0.13}$ $0.12^{+0.13}_{-0.06}$	$0 . 28_{- 0.2}^{+ 0.32}$ $0.28^{+0.32}_{-0.2}$	–
GW190720_000836; [3]	$0 . 63_{- 0.27}^{+ 0.31}$ $0.63^{+0.31}_{-0.27}$	$0 . 17_{- 0.11}^{+ 0.13}$ $0.17^{+0.13}_{-0.11}$	$0 . 3_{- 0.21}^{+ 0.35}$ $0.3^{+0.35}_{-0.21}$	–
GW191204_171526; [4]	$0 . 7_{- 0.26}^{+ 0.26}$ $0.7^{+0.26}_{-0.26}$	$0 . 16_{- 0.05}^{+ 0.08}$ $0.16^{+0.08}_{-0.05}$	$0 . 39_{- 0.26}^{+ 0.36}$ $0.39^{+0.36}_{-0.26}$	–
GW190708_232457; [3]	$0 . 75_{- 0.28}^{+ 0.22}$ $0.75^{+0.22}_{-0.28}$	$0 . 02_{- 0.08}^{+ 0.1}$ $0.02^{+0.1}_{-0.08}$	$0 . 3_{- 0.24}^{+ 0.43}$ $0.3^{+0.43}_{-0.24}$	–
GW190930_133541; [3]	$0 . 66_{- 0.37}^{+ 0.28}$ $0.66^{+0.28}_{-0.37}$	$0 . 14_{- 0.14}^{+ 0.2}$ $0.14^{+0.2}_{-0.14}$	$0 . 33_{- 0.23}^{+ 0.38}$ $0.33^{+0.38}_{-0.23}$	-
GW191216_213338; [4]	$0 . 63_{- 0.28}^{+ 0.31}$ $0.63^{+0.31}_{-0.28}$	$0 . 11_{- 0.06}^{+ 0.13}$ $0.11^{+0.13}_{-0.06}$	$0 . 23_{- 0.16}^{+ 0.33}$ $0.23^{+0.33}_{-0.16}$	–
GW190707_093326; [3]	$0 . 73_{- 0.22}^{+ 0.22}$ $0.73^{+0.22}_{-0.22}$	$- 0 . 03_{- 0.07}^{+ 0.08}$ $-0.03^{+0.08}_{-0.07}$	$0 . 25_{- 0.2}^{+ 0.38}$ $0.25^{+0.38}_{-0.2}$	–
GW190512_180714; [3]	$0 . 54_{- 0.18}^{+ 0.37}$ $0.54^{+0.37}_{-0.18}$	$0 . 03_{- 0.13}^{+ 0.13}$ $0.03^{+0.13}_{-0.13}$	$0 . 23_{- 0.18}^{+ 0.35}$ $0.23^{+0.35}_{-0.18}$	–
GW191103_012549; [4]	$0 . 67_{- 0.36}^{+ 0.29}$ $0.67^{+0.29}_{-0.36}$	$0 . 21_{- 0.1}^{+ 0.16}$ $0.21^{+0.16}_{-0.1}$	$0 . 4_{- 0.28}^{+ 0.4}$ $0.4^{+0.4}_{-0.28}$	–
GW170608; [5]	$0 . 7_{- 0.37}^{+ 0.27}$ $0.7^{+0.27}_{-0.37}$	$0 . 03_{- 0.07}^{+ 0.19}$ $0.03^{+0.19}_{-0.07}$	$0 . 35_{- 0.27}^{+ 0.44}$ $0.35^{+0.44}_{-0.27}$	–
GW190725_174728; [3]	$0 . 57_{- 0.31}^{+ 0.38}$ $0.57^{+0.38}_{-0.31}$	$- 0 . 04_{- 0.14}^{+ 0.26}$ $-0.04^{+0.26}_{-0.14}$	$0 . 37_{- 0.29}^{+ 0.46}$ $0.37^{+0.46}_{-0.29}$	–
GW200225_060421; [4]	$0 . 73_{- 0.28}^{+ 0.24}$ $0.73^{+0.24}_{-0.28}$	$- 0 . 11_{- 0.28}^{+ 0.16}$ $-0.11^{+0.16}_{-0.28}$	$0 . 53_{- 0.38}^{+ 0.34}$ $0.53^{+0.34}_{-0.38}$	e.g. Antonelli et al. (2023), Zhang et al. (2023)
GW191105_143521; [4]	$0 . 71_{- 0.3}^{+ 0.25}$ $0.71^{+0.25}_{-0.3}$	$- 0 . 02_{- 0.09}^{+ 0.13}$ $-0.02^{+0.13}_{-0.09}$	$0 . 29_{- 0.24}^{+ 0.46}$ $0.29^{+0.46}_{-0.24}$	–
GW151012; [6]	$0 . 59_{- 0.35}^{+ 0.36}$ $0.59^{+0.36}_{-0.35}$	$0 . 05_{- 0.21}^{+ 0.3}$ $0.05^{+0.3}_{-0.21}$	$0 . 34_{- 0.26}^{+ 0.45}$ $0.34^{+0.45}_{-0.26}$	–
GW191129_134029; [4]	$0 . 63_{- 0.3}^{+ 0.31}$ $0.63^{+0.31}_{-0.3}$	$0 . 06_{- 0.08}^{+ 0.16}$ $0.06^{+0.16}_{-0.08}$	$0 . 26_{- 0.2}^{+ 0.37}$ $0.26^{+0.37}_{-0.2}$	–
GW200202_154313; [4]	$0 . 72_{- 0.31}^{+ 0.24}$ $0.72^{+0.24}_{-0.31}$	$0 . 04_{- 0.06}^{+ 0.12}$ $0.04^{+0.12}_{-0.06}$	$0 . 28_{- 0.21}^{+ 0.41}$ $0.28^{+0.41}_{-0.21}$	–

Notes. We provide the 90% credible intervals for the mass ratio (q), effective inspiral spin (χ_eff), and effective precession spin (χ_p) of events for which the median of the mass posterior distribution (for one or both components) lies above 10 M_⊙ for events with ℳ < 11 M_⊙ and below 15 M_⊙ for events with ℳ > 11 M_⊙. The events are ordered from having the most to least posterior support in the gap. We include the publication where the event is first reported: [1] Abbott et al. (2020); [2] Abbott et al. (2016b); [3] Abbott et al. (2021a); [4] Abbott et al. (2023a); [5] Abbott et al. (2017); [6] Abbott et al. (2016a); and some studies that have suggested a formation scenario different from isolated binary evolution for a given system.

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