Translating inferences between eccentric gravitational waveform models

Orbital eccentricity is a key signature of dynamical binary black hole (BBH) formation. The gravitational waves from a coalescing binary contain information about its orbital eccentricity, which can be measured if the binary retains sufficient eccentricity close to merger. Measurements of eccentricity require accurate inspiral-merger-ringdown waveform models that incorporate eccentric dynamics. Several models are in good agreement with numerical relativity and have been used to constrain the eccentricities of BBH candidates detected during the first three LIGO/Virgo observing runs. However, these models define eccentricity in disparate ways, posing a challenge to obtaining meaningful eccentricity measurements. We present studies that map these conflicting waveform definitions to each other, and show how this information can be leveraged for parameter estimation.