Eccentricity estimate for black hole mergers with numerical relativity simulations

The origin of black hole mergers discovered by the LIGO1 and Virgo2 gravitational-wave observatories is currently unknown. GW1905213,4 heaviest merger detected so far. Its observed high mass possible spin-induced orbital precession could arise from binary having formed following a close encounter. An observational signature encounters eccentric orbit5–7; however, this feature difficult to identify due lack suitable gravitational waveforms. No has been previously found8. Here we report 611 numerical relativity simulations covering full eccentricity range an estimation approach probe mergers. Our set corresponds ~105 waveforms, comparable number used in searches, albeit with coarser ratio spin resolution. We applied our GW190521 found that it most consistent highly ( $$e=0.6{9}_{-0.22}^{+0.17}$$ ; 90% credible level) within This interpretation supported over non-eccentric >10 odds if ?10% GW190521-like are eccentric. Detectable would be evidence against isolated origin, which otherwise rule out on basis spin9,10. Massive holes produced dynamically thought involve orbits, whose imprint may remain waveform LIGO/Virgo Collaboration.