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Most gravitational wave (GW) events observed by the LIGO and Virgo detectorsare consistent with mergers of binary black holes (BBHs) on quasi-circularorbits. However, some events are also consistent with non-zero orbitaleccentricity, which can indicate that the binary formed via dynamicalinteractions. Active GW search pipelines using quasi-circular waveformtemplates are inefficient for detecting eccentric mergers. Also, analysingeccentric GW signals with waveform models neglecting eccentricity can lead tobiases in the recovered parameters. We explore the detectability andcharacterisation of eccentric signals when searches and analyses rely onquasi-circular waveform models. We find that for a reference eccentricpopulation, the fraction of events having fitting factor (FF) $< 0.95$ can beup to $\approx 2.2\%$ compared to $\approx 0.4\%$ for the baseline population.This leads to the loss in signal recovery fraction for up to $6\%$ forparameter space with non-negligible eccentricity ($e_{10} > 0.01$) and highmass ratio ($q > 3$). We perform parameter estimation (PE) for non-spinning andaligned-spin eccentric GW injections from BBHs with a total mass $M=35M_\odot$, based on numerical relativity simulations and an EOB basedinspiral-merger-ringdown model (TEOBResumS). We recover these injections usingboth quasi-circular and eccentric waveform models. For cases with $e_{20} \sim0.1$, quasi-circular models fail to estimate chirp mass within the 90% credibleinterval accurately. Further, for these low-mass injections, spin-inducedprecession does not mimic eccentricity. For injections of $e_{20}\sim 0.1$, PEconducted with an inspiral-only eccentric waveform model correctlycharacterises the injected signal to within 90% confidence, and recovers theinjected eccentricities, suggesting that such models are sufficient forcharacterisation of low-mass eccentric BBH. (abridged)

Blind spots and biases: the dangers of ignoring eccentricity in gravitational-wave signals from binary black holes