Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA

Binary black holes (BBHs) in eccentric orbits produce distinct modulations the emitted gravitational waves (GWs). The measurement of orbital eccentricity can provide robust evidence for dynamical binary formation channels. We analyze 57 GW events from the first, second and third observing runs of the LIGO-Virgo-KAGRA (LVK) Collaboration using a multipolar aligned-spin inspiral-merger-ringdown waveform model with two eccentric parameters: eccentricity and relativistic anomaly. This is made computationally feasible with the machine-learning code DINGO which accelerates inference by 2-3 orders of magnitude compared to traditional inference. First, we find eccentric aligned-spin versus quasi-circular aligned-spin ₁₀ Bayes factors of 1. 84 to 4. 75 (depending on the glitch mitigation) for GW200129, 3. 0 for GW190701 and 1. 77 for GW200208₂2. We measure e₆ₖ, ₁₀₇ₙ to be 0. 27-₀. ₁₂^+0. 10 to 0. 17-₀. ₁₃^+0. 14 for GW200129, 0. 35-₀. ₁₁^+0. 32 for GW190701 and 0. 35-₀. ₂₁^+0. 18 for GW200208₂2. Second, we find ₁₀ Bayes factors between the eccentric aligned-spin versus quasi-circular precessing-spin hypothesis between 1. 43 and 4. 92 for GW200129, 2. 61 for GW190701 and 1. 23 for GW200208₂2. Third, our analysis does not show evidence for eccentricity in GW190521, which has an eccentric aligned-spin against quasi-circular aligned-spin ₁₀ Bayes factor of 0. 04. Fourth, we estimate that if we neglect the spin-precession and use an astrophysical prior, the probability of one out of the 57 events being eccentric is greater than 99. 5% or (100 - 8. 4 10^-4) % (depending on the glitch mitigation). Fifth, we study the impact on parameter estimation when neglecting either eccentricity or higher modes in eccentric models. These results underscore the importance of including eccentric parameters in the characterization of BBHs for GW detectors.