  Detecting binary black hole (BBH) mergers with quantifiable orbital
eccentricity would confirm the existence of a dynamical formation channel for
these binaries. The current state-of-the-art gravitational wave searches of
LIGO-Virgo-KAGRA strain data focus more on quasicircular mergers due to
increased dimensionality and lack of efficient eccentric waveform models. In
this work, we compare the sensitivities of two search pipelines, the matched
filter-based \texttt{PyCBC} and the unmodelled coherent Wave Burst
(\texttt{cWB}) algorithms towards the spinning eccentric BBH mergers, using a
multipolar nonprecessing-spin eccentric signal model, \texttt{SEOBNRv4EHM}. Our
findings show that neglecting eccentricity leads to missed opportunities for
detecting eccentric BBH mergers, with \texttt{PyCBC} exhibiting a $10-20\, \%$
sensitivity loss for eccentricities exceeding $0.2$ defined at $10$ Hz. In
contrast, \texttt{cWB} is resilient, with a $10\, \%$ sensitivity increase for
heavier ($\mathcal{M} \ge 30 \, \text{M}_{\odot}$) eccentric BBH mergers, but
is significantly less sensitive than \texttt{PyCBC} for lighter BBH mergers.
Our fitting factor study confirmed that neglecting eccentricity biases the
estimation of chirp mass, mass ratio, and effective spin parameter, skewing our
understanding of astrophysical BBH populations, fundamental physics, and
precision cosmology. Our results demonstrate that the current search pipelines
are not sufficiently sensitive to eccentric BBH mergers, necessitating the
development of a dedicated matched-filter search for these binaries. Whereas,
burst searches should be optimized to detect lower chirp mass BBH mergers as
eccentricity does not affect their search sensitivity significantly.
