  The problem of gravitational wave parameter estimation and source
localization is crucial in gravitational wave astronomy. Gravitational waves
emitted by compact binary coalescences in the sensitivity band of
second-generation ground-based detectors could have non-negligible
eccentricities. Thus it is an interesting topic to study how the eccentricity
of a binary source affects and improves the accuracy of its localization (and
the signal-to-noise ratio). In this work we continue to investigate this effect
with the enhanced postcircular waveform model. Using the Fisher information
matrix method, we determine the accuracy of source localization with three
ground-based detector networks. As expected, the accuracy of source
localization is improved considerably with more detectors in a network. We find
that the accuracy also increases significantly by increasing the eccentricity
for the large total mass ($M\ge 40M_\odot$) binaries with all three networks.
For the small total mass ($M<40 M_\odot$) binaries, this effect is negligible.
For the smaller total mass ($M<5 M_\odot$) binaries, the accuracy could be even
worse at some orientations with increasing eccentricity. This phenomenon comes
mainly from how well the frequency of the higher harmonic modes induced by
increasing eccentricity coincides with the sensitive bandwidth of the
detectors. For the case of the $100 M_\odot$ black hole binary, the improvement
factor is about $2$ in general when the eccentricity grows from $0.0$ to $0.4$.
For the cases of the $22 M_\odot$ black hole binary and the $2.74 M_\odot$
neutron star binary, the improvement factor is less than $1.1$, and it may be
less than 1 at some orientations.
