  Utilizing publicly available non-spinning eccentric binary black hole (BBH)
merger simulations
(\href{https://data.black-holes.org/waveforms/catalog.html}{https://data.black-holes.org/waveforms/catalog.html})
from the SXS collaboration~\cite{Hinder:2017sxy}, we present convincing
evidence that the waveform phenomenology in eccentric BBH mergers is
significantly simpler than previously thought. We find that the eccentric
modulations in the amplitudes, phases, and frequencies in different spherical
harmonic modes are all related and can be modeled using a single time series
modulation. Using this universal eccentric modulation, we provide a model named
\texttt{gwNRHME} to seamlessly convert a multi-modal (i.e with several
spherical harmonic modes) quasi-circular waveform into multi-modal eccentric
waveform if the quadrupolar eccentric waveform is known. This reduces the
modelling complexity of eccentric BBH mergers drastically as we now have to
model only a single eccentric modulation time-series instead of modelling the
effect of eccentricity in all modes. When compared with the NR simulations, our
model mismatches are mostly $\sim 10^{-3}$ and are comparable to the numerical
errors in the NR simulations. Our method is modular and can be readily added to
any quadrupolar non-spinning eccentric waveform model. We make our model
publicly available through the \texttt{gwModels}
(\href{https://github.com/tousifislam/gwModels}{https://github.com/tousifislam/gwModels})
waveform package.
