  Effective one body numerical relativity waveform models for spin aligned
binary black holes (SEOBNR) are based on the effective one body theoretical
framework and numerical relativity simulation results. SEOBNR models have
evolved through version 1 to version 4. We recently extended SEOBNRv1 model to
SEOBNRE (Effective One Body Numerical Relativity waveform models for Spin
aligned binary black holes along Eccentric orbit) model which is also valid for
spin aligned binary black hole coalescence along eccentric orbit. In this paper
we update our previous SEOBNRE model to make it consistent to SEOBNRv4 which is
the most widely used SEOBNR waveform model. This upgraded SEOBNRE model
improves accuracy compared to previous SEOBNRE model, especially for highly
spinning black holes. For spin aligned binary black holes with mass ratio
$1\leq q\lesssim10$, dimensionless spin $-0.9\lesssim\chi\lesssim0.995$ and
orbital eccentricity $0\leq e_0\lesssim0.6$ at reference frequency $Mf_0=0.002$
($M$ is the total mass of the binary black hole, $f_0\approx 40\frac{10{\rm
M}_\odot}{M}$Hz), the upgraded SEOBNRE model can always fit numerical
relativity waveform better than 98.2\%. For most cases the fitting factor can
even be better than 99\%.

General Relativity and Quantum Cosmology